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TJcpartmcnt of Astronomy 

UNn^ERSITV OF TORONTO 




Kepler 
i6og 



No. 



PUBLICATIONS OF 

THE DAVID DUNLAP OBSERVATORY 

UNIVERSITY OF TORONTO 

VOLUME 3 



1 Period changes of RR Lyrae variables in the globular cluster 
Messier 5 Christine M. Coutts, Helen Sawyer Hogg 

2 Studies of the variables in the globular cluster NGC 6171 

Christine M. Coutts, Helen Sawyer Hogg 

3 Variables in Messier 5: A study of Mount Wilson 

1917 observations Christine M. Coutts 

4 Spectroscopic orbits of the binary systems HD 128661, AR Cas, 
beta Ari and HD 209813 Walter L. Gorza, John F. Heard 

5 The establishment of 21 new ninth magnitude lAU standard radial 
velocity stars John F. Heard, CH. Fehrenbach 

6 A third catalogue of variable stars in globular clusters 
comprising 2119 entries Helen Sawyer Hogg 

7 The Sculptor dwarf spheroidal galaxy I. Discovery and 
identification of variable stars S.L. Th. J. Van Agt 



PUBLICATIONS OF 

THE DAVID DUNLAP OBSERVATORY 

UNIVERSITY OF TORONTO 

Volume 3 Number 1 



PERIOD CHANGES OF RR LYRAE 

VARIABLES IN THE GLOBULAR 

CLUSTER MESSIER 5 



CHRISTINE M. COUTTS 

AND 
HELEN SAWYER HOGG 



1969 
TORONTO, CANADA 



PUBLICATIONS OF 

THE DAVID DUXLAP OBSERVATORY 

UNIVERSITY OF TORONTO 

Volume 3 Number 1 



PERIOD CHANGES OF RR LYRAE 

VARIABLES IN THE GLOBULAR 

CLUSTER MESSIER 5 



CHRISTINE AI. COUTTS 

AND 
HELEN SAWYER HOGG 



1969 
TORONTO, CANADA 



JUN im 

%5s/ry OF ^^^ 



PRINTED AT 
THE UNIVERSITY OF TORONTO PRESS 



PERIOD CHANGES OF RR LYRAE VARIABLES 
IN THE GLOBULAR CLUSTER MESSIER 5 

By Christine 'SI. Coutts and Helen Sawyer Hogg 



Abstract 

The purpose of this investigation is to study period changes in RR Lyrae variables 
in the globular cluster M5. The study is based mainly on a collection of 167 plates 
taken between 1936 and 1966 at the David Dunlap Observatory. Some 64 photo- 
graphs taken by Dr. Harlow Shapley in 1917 with the 60-inch telescope on Mount 
Wilson have also been measured. 

Studies of this type which have been carried out for other globular clusters are 
briefly discussed. The methods for studying period changes using a phase-shift 
diagram are explained. 

A total of 66 RR Lyrae variables has been studied in Mo. Of these, 16 have 
irregular periods, 18 have been constant, 20 have shown increases (median rate 
0.05 =fc 0.02 days per million years) and 12 decreases (median 0.075 ± 0.02 days per 
million years) in period during an interval of about seventy years. It seems not 
possible at present to attach any evolutionary significance to these changes. 

Introduction 

Messier 5 is in third place among the globular clusters which are 
richest in variable stars (co Centauri and Messier 3 supersede it). The 
only study of period changes of the RR Lyrae variables in this cluster 
was made 27 years ago by Oosterhofif (1941), based on oI)servations 
obtained up to the year 1935. Messier 5 is therefore a cluster very 
suitable for a study of changes in period. One of us (Sawyer Hogg) has 
taken a series of 13G photographs of this cluster witli the 74-inch 
telescope between 1936 and 1964 inclusive. 

An additional series of 31 plates was taken by Coutts on four nights 
in 1966 with the 74-inch telescope at the David Dunlap Observatory, 
after this investigation was begun. Dr. H. W. Babcock kindly lent us 
some plates taken by Dr. Harlow Shapley with the 60-inch telescope 
at Mount Wilson Observatory in 1917. Although these plates were 
studied previously (Shapley 1927), the individual observations were 
never published and so these plates were remeasured. The measures of 
the David Dunlap and Mount Wilson plates form the basis for the 
present investigation. 

In addition, a number of published observations of the variables in 
M5 are available, from 123 photographs taken between 1889 and 1912 
by Bailey (1917), and from 81 photographs with the 60-inch Mount 



4 Christine M. Coiitts and Helen Sawyer Hogg 

Wilson telescope in 1934 and 1935 by Oosterhoff (1941). When all this 
material is considered, M5 can be studied over an interval of more 
than seventy years. It is important to find what characteristics of the 
period changes of the RR Lyrae variables in AI5 are similar to those in 
the other clusters which have been studied already. 

Other Studies oj the Period Changes of RR Lyrae Variables in 
Globular Clusters 

About ten globular clusters have been investigated for period 
changes. The results, on the wiiole, do not indicate any particular 
trend in changes in period of the RR Lyrae stars. Some variables have 
constant periods. Some have periods which are secularly decreasing 
and others Avhich are secularly increasing. In most clusters, there 
appears to be no preference for periods to increase or decrease. The 
clusters which have been investigated specifically for period changes 
are listed in Table I, in order of decreasing number of variables. 





TABLE I 


Cluster 


No. of 
RR Lyrae 
Variables 


Investigators 


NGC 5272 = M3 


173: 


Martin (1942) 
Hett (1942) 
Belserene (1952) 
Ozsvath (1957) 
Szeidl (1965) 
Kheylo (1966) 


NGC 5139 = CO Centaiiri 


140: 


Martin (1938) 
Belserene (1961, 1964) 


NGC 5904 = Mo 


93 


Oosterhoff (1941) 


NGC 7078 = M15 


88 


Izsak (1956) 

Mannino (1956a, 1956b) 

Grubissich (1956) 

Nobili (1957) 

Notni and Oleak (1958) 

Bronkalla (1959) 

Fritze (1962) 

Makarova and Akimova (1965) 


NGC 6402 = M14 


69: 


Sawyer Hogg and Wehlau (1968) 


NGC 6121 = M4 


41 


Wilkens (1964) 


NGC 5024 = M53 


38: 


Margoni (1964, 1965a, 1965b, 1967) 
W'achmann (1965) 


NGC 5466 


18 


Bartolini, Biolchini and 
Mannino (1965) 


NGC 7089 


13 


Mantegazza (1961) 
Kulikov (1961) 


NGC 6341 = M92 


12 


Kheylo (1964, 1965) 

Bartolini, Battistini and Nasi (1968) 


NGC 5053 


10 


Mannino (1963) 



Period Changes of liR Lyrae Variables in Mo 5 

The RR L\Tae stars in w Centauri exhibit a distinct tendency for the 
periods to increase. For about 70 per cent of the stars investigated in 
this cluster, the periods show secular increases while the others 
decrease, remain constant or fluctuate. The median rate of change of 
period for 47 variables classed as RR a,b types investigated by 
Belserene (1964) is an increase of 0.11 days per million years. 

The RR Lyrae variables in M3, on the other hand, do not exhibit 
such a tendency. Szeidl (1965) has studied 112 variables. Of these, 22 
have periods which are increasing at an average rate of 0.18 days per 
million years and 25 have periods which are decreasing at an average 
rate of 0.20 days per million Aears. Of the other periods, 7 have re- 
mained constant and the rest are fluctuating. The average rate of 
change of period of all the stars is a decrease of 0.02 days per million 
years, but the median rate is zero. Thus the RR Lyrae variables in M3 
behave in a different manner from those in co Centauri. Belserene 
(1964) has pointed out, however, that the period-amplitude relations 
for tliese two clusters are also different, and therefore she notes that 
conclusions based on the observations of RR Lyrae variables in one 
cluster are not necessarily applicable to the class of variables as a whole. 

In A 115, there are a few more stars with increasing periods than with 
decreasing, hut the tendency,' to increase is not as marked as that in 
oj Centauri. 

In the other clusters investigated, there are approximately equal 
numbers of stars with increasing and decreasing periods. Margoni 
(1967) in his work on A 153 has suggested that sine curves can be fitted 
to the phase-shift diagrams for five of the stars on tlie basis of the 
present observations. This implies tliat the period changes are periodic 
and if this be true, we can not attach any evolutionary significance to 
the values of /3 computed for otlier stars. The quantity /3 is the rate of 
change in the period in days per day as defined by Martin (1938). 

For A15, Oosterhoff (1941) used observations from 1895, 1896, 1897, 
1912, 1917, 1934 and 1935. He considered 41 stars of RR Lyrae types 
a, b and found that the average period change was an increase of 0.05 
days per million years, with 25 periods increasing and 15 decreasing, 
and 1 remaining constant. The tendency for periods to increase is 
therefore not as marked as in w Centauri. 

Theory of Investigation of Period Changes 

To investigate changes in period among RR Lyrae stars, a reason- 
ably accurate period is needed, i.e., it must satisfy the observations 
over an interval of one or two years. The light curve is derived by 
reducing all the observations of the star to one cycle of light variation. 



Christine M. Coutts and Helen Sawyer Hogg 




Fig. 1 — Light curve of an RR Lyrae variable (phase in fractions of period). 

A certain period, P, is assumed and a reference epoch at time E is 
adopted. All the observations at the different times, /, are reduced to 
one cycle of period, P, at epoch E, such that: phase = {t — E)/P. 
This is the number of cycles of length P, which have elapsed between 
epoch E and time /. The phase adopted at time / is the fractional part 
of this number. When phases are computed at a series of times /, a 
light curve can then be plotted. If the period is constant and correct, 
the scatter on the light curve should be that expected from the 
accuracy of the observations. However, if the scatter is larger than this, 
the assumed period is incorrect or varying or both. The method used 
to examine the behaviour of the period is to plot a phase-shift diagram. 
There are five cases of the phase-shift diagram, described below. 



Case 1: Assumed period incorrect 

Suppose that the true period is a, and that an incorrect value P has 
been assumed in computing the phase for the light curve. Then the 
resulting displacement in phase is given by: 



A phase = 



t - E 



where AP = a — P. 



= (/-£) 

__ {t - E) 
- P' 



- P 
Pa 



AP, 



If A phase is plotted against /, a straiglit line results, and the true 
period can be determined from the slope of this line, AP/ P^. 



Case 2: Period changing at a uniform rate 

Suppose that the period is not constant, but instead, changes at a 
constant rate /3. If the period at time E is a, then the period at time t is 



Period Changes of RR Lyrac Vnriahles in Mo 





TIME 



TIME 



TIME 



Fig. 2 — Phase-shift diagrams for a star of constant period: (a) a, the true period, 
> P, the assumed period (b) a < P, {c) a = P. 

given by: P = a + jS(/ — E). Since the period is changing at a con- 
stant rate, the true phase at time t should be given by: 

/ - E 



a + I (/ - £) 

The phase calculated assuming a constant period, a, is: (/ — E)/a. 
Hence, the displacement in phase (or phase-shift) at time / is: 



A phase = 

a 



t - E 



« + !(/-£)' 



/ - E 
a 



Li-{i-£(^-^)fj 



^(t - E Y 
2a- 



/•here ^ ■ (/-£)«!. 
Za 



In this case, if A phase is plotted against /, the result is a paral)ola with 
a vertical axis, with equation: 

A pliase = A + Bt + Ct^ 

where C = 13/ 2 P- day"'-. If the parabola is concave upward, /3 is 
positive, and the period is increasing. If the parabola is concave 
downward, the period is decreasing. 

Case 3: Assumed period incorrect and period changing at a uniform 
rate 

Suppose that the assumed period is not the true period at time E 
and that the period is changing at a constant rate. Indeed, if the 



Christine M. Coutts and Helen Sawyer Hogg 





TIME 



TIME 



Fig. 3 — Phase-shift diagrams for a star with period changing at a uniform rate: 
(a) /3 > 0, period increasing; (b) /? < 0, period decreasing. 

period is changing, it is very difficult to determine the period precisely 
at any given moment. In this case, the phase shift at time / is given by: 



A phase = 



t - E 
P 



E 



& 



t - E t - E t - E 



P 



t - E 
a 



a + f (/ - £) 



+ 



/ - E 



^^(/-E)+^,(/-£)^ 

Thus, a plot of A phase against time once again results in a paral)ola 
witli a vertical axis (see figure 3). The value of /3 is again determined 
from tlie coefficient of the /- term /3/2P-. 

Case 4: An abrupt change in period 

If the period changes al)ruptly, rather than gradually, the phase- 
shift diagram consists of two straight lines with different slopes. If the 



TIME 



Fig. 4 — Phase-shift diagram for a star whose period changes abruptly. 



Period Changes of lUi Lyrae Variahles in Md 9 

slope of the second line is greater than that of the first, an increase in 
period is indicated. The amount of change in tlie period is related to 
the difference in slope l)et\veen the two lines: \P = (A slope) P-. 

Case 5: Irregular changes in period 

Many phase-shift diagrams have a more complicated form than 
those described above. In such cases, it is difficult to predict long-range 
period changes. An increase in slope indicates an increase in period and 
a decrease in slope, a decrease in period. However, if these changes 
occur in an irregular manner, it must lie assumed that the period 
changes are random. 

Obviously the phase-shift diagram can give important information 
regarding the behaviour of the period of a star. In the past, most 
investigators have assumed a parabolic form for the phase-shift 
diagram (rather than a more complicated curve) to determine the 
period change. According to Belserene (196-1), (3 is a. useful parameter 
for describing the extent of the variation in period. She adds, "It is the 
average rate of period change if the true rate lias \-aried." However, 
Makarova and Akamova (19G5) in a study of RR Lyrae variables of 
Alio find that for about 50 per cent of the stars they studied, the 
period changes are abrupt, i.e., the phase-shift diagram is represented 
better by two intersecting straight lines than In' a parabola. This is also 
a simple assumption, but it is difficult to determine the rate of period 
change when the observed quantity is its amount. 

In the present investigation, the period change is determined by 
both methods. 

Present Investigation 

The globular cluster A 1 5 lias a total of 98 variables (Init tlie vari- 
ability of one, no. 51, is questionable). There are two W V'irginis 
variables (nos. 42 and 84), one irregular (no. 50), one SS C^'gni (no. 
101) and 93 RR Lyrae. Of the RR Lyrae stars, 91 have periods 
determined (Bailey 1917, Shapley 1927, and Oosterhoft" 1941). Sixty- 
eight are of type a, b and twenty-three are type c. 

The plates used with the 74-inch reflector were Eastman Kodak 
103aO. Sixty-six RR Lyrae stars (50 of type a, b and 16 of type c) and 
the two \V Virginis stars could be studied on tliese plates. Most of the 
stars were measured with a Cuft"e>- iris astrophotometer, but the 
magnitudes of variables 6, 13, 14, 27, 33, 34, 38, 45, 63, 67, 69, 83 and 
98 were estimated by e\e. 

A sequence of [photoelectric li, V standards determined bv Arp 



10 



Christine M. Coutts and Helen Sawyer Hogg 



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Period Changes of RR Lyrae Variables in M5 



11 



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12 Christine M. Contts and Helen Sawyer Hogg 

(1962) was used to reduce the data. Arp's B magnitudes were converted 
to photographic magnitudes by his relations: 

B = Wpg + 0.23 - 0.16 CI 

V = nip^ 

CI = ntpg — ?;Zpv. 

In addition, each plate was examined for the visibility of an SS Cygni 
star discovered by Oosterhoff (19-41), but it was not detected. The 
limiting magnitude of many of the David Dunlap plates, whose 
exposure times average onh' 3 minutes, is at a brighter magnitude than 
the maxinumi, ;;?pg == 17.16, at which Oosterhofif observed this star. 
The observations (photographic magnitudes) are listed in Table III 
where the first column gives the plate number (for variables 1-27), and 
the second column the heliocentric Julian da},' \\ith the first two digits 
(24) omitted. In subsequent sections of the tal)le the plate numbers 
are not repeated. Measures could be made on 157 plates. 

Thirty-three plates taken by Shaple},- in 1917 with the 60-inch 
Mount Wilson telescope were also measured. Some of the plates had 
two exposures of the cluster so that there were 64 photographs alto- 
gether, with exposures usually 2 or 3 minutes. All tlie variable stars 
except variables 6, 33, and 38 were measured with the iris photometer, 
while the others were estimated visually. Some of the stars measured 
on the David Dunlap plates (variables 13, 27, 84 and 98) could not be 
measured on the Mount Wilson plates owing to the double exposures 
on the latter. The presence of two exposures on one plate has the effect 
of crowding the field, particularh- in the nuclear region of the cluster. 
The observations (photographic magnitudes) from the Mount Wilson 
plates are listed in Table IV. The first column gives the Mount Wilson 
plate number for the 32 plates whose quality- permitted measures, and 
the second column gives the heliocentric Julian day with the first two 
digits (24) omitted. From these two columns the plates witli two 
exposures can be identified. We made ever\' efiort to determine which 
exposure was made first, but we cannot guarantee that the decision is 
always correct. Tlie time difference between the two exposures is so 
small that we used the means of the times and of the magnitudes. 

On both series of plates, no correction was made for background 
light whicli has the efifect of making the stars in dense regions of the 
cluster appear too bright. There are no photoelectric standards in 
these regions, and correction for background intensity without such 
standards could introduce additional uncertainties into the results. 

These two series, totalling 200 plates, along with the values from 123 



TABLE III 

Photographic [Magnitudes from the David Duxlap Plates 



14 



Plate 

819 
828 
829 
830 
831 
838 
1107 
1122 
1285 
1976 
1990 
2005 
2012 
2029 
2108 
3246 
3259 
3269 
3284 
3296 
3310 
3325 
5706 
5720 
5804 
5817 
5832 
5839 
6855 
6868 
7852 
7867 
7935 
7952 
7971 
7989 
8008 
8115 
8801 
8804 
8807 
8810 
8813 
8816 
8819 
8827 
8830 
8833 
8836 
8839 
8842 



Julian Day 

28308.736 

8309.651 

.661 

.670 

.677 

.796 

8365.608 

8366.608 

8399.596 

8688.640 

8089.640 

8692.632 

8693,730 

8696.631 

8715.638 

9071.660 

9072.698 

9073.605 

9076.603 

9077.600 

9078.600 

9079.602 

9786.609 

9787.608 

9813.610 

9814.612 

9815.613 

9816.611 

30171.617 

0172.615 

0519.606 

0520.606 

0550.608 

0553.604 

0554.614 

0555.629 

0556.620 

0586.572 

0880.592 

.623 

.659 

.690 

.730 

.760 

.788 

0883.593 

.630 

.664 

0884.622 

.651 

.680 



TABLE III. PHOTOGRAPHIC ALAGNITLlDES FE 
No. 1 No. 2 No. 3 No. 6 No. 7 No. 8 No. 9 No 



15.3 
15. 25 
15.28 

15.45 

15.4 

15.39 



15. 
15. 
14. 



3 

4 
55 



15.47 
15.42 
15.34 



14.68 

14.56 

15.45 

15.4 

15.41 

15.48 

15.44 

15.52 

15.44 

15. 53 

15.41 

14.97 

15.06 

15.32 

15.39 

15.39 

14.75 

15.49 

15.22 

15.4 

15.36 

15.1 



15.29 
15,47 



15.17 14.74 15.05 15.3 



15. 19 
15.29 
15.43 
15.43 
15.39 
14.81 



15.42 
15. 5 
15.62 
15.58 

15.47 

15.44 

15.6 

15.58 

15.25 

15. 58 

15.37 

15.4 

15.81 

15.44 

15.21 

15.02 

15.53 
15.54 

14.15 
14.46 



15.54 
15.66 



14.76 
14.86 
15. 11 
15. 17 
15.39 
15.38 



15.48 14.97 

15.5? 15.21 

14.77 15.51 

15.51 15.41 

15.47 15.3 

15.23 15.33 



15.45 
15.43 



,45 
,45 



15.05 
15.44 
15.21 
14.96 
14.84 
15.39 
15.47 
15.41 
15.15 
14.92 



15. 
15. 



45 
3 



15.0 

14.85 

14.85 

15.25 

14.9 

14.85 

14.6 

14.9 

14.85 

15.05 

14.5 
15.05 
15.05 
14.0: 



15.0: 
14.96 
14.76 
14.53 
14.66 
15. 56 



35 

,45 
,50 



15.31 15.15: 



15.25 

15.25 

15.25 

15.3 

15.15 

14.85 

14.6 



14.5 

14.9 

14.55 

15.25 

14.85 

14.4 

15.25 
15.0 



14.78 
15.27 

14.74 



15.01 

15.12 

15.43 

15.31 

15.01 

14.75 

14.4 

14.41 

15.40 

15.41 

15.37 

15.43 

15.66 

15.45 
15.28 



15.33 14.6 

15.36 14.85 

15.43 14.9 

15.44 14.95 



14.55 
15.0 
14.92 
15.11 



15.6 

15.48 

15.42 

14.65 

15.20 

14.76 

15.40 



15.35 
15.35 
15.21 

15.43 
15.44 
15.3 



15.51 

15.54 

14.95 

15.13 

15. 56 

15. 5 

15. 5 

15.4 

15.28 

15.42 

15.23 

15. 5 

15.75 

15.56 

15.40 

15.05 



15.43 14.4 14.57 15. 



15.43 
15.49 
15.50 
15. 55 



14.80 14.9] 
14.89 
14.97 
15.18 



15.02 
15.36 
15.36 



15.27 

15.63 

14.65 

15.36 

15.36 

15.23 

15.1 

15.39 

14.74 

15.37 



44 
49 



15.27 
15.45 
14.87 
14.56 



15. 



14.82 15.5 

15.31 15.5; 

15.54 15.1 

15.3 15.6; 

15.25 15.4 

15.01 15.5 



15.21 15.45 15.6 



15. 



15.3 
15.5 
15.4 
15.6 
15. £ 
15. £ 
15. S 
15. f 
15. < 
15.] 
15.^ 
14. J 
15. i 



15.42 15. { 

15.27 15.; 

15.45 15. i 

15.35 14.! 

15.0 14. ( 



15.31 15.1 14.71 14.67 14.55 15. 
15.41 15.25 15.05 14.9 14.74 15. 



15.41 15.64 15.35 15.25 15.19 14.80 15.32 15. 



15 

THE DAVID DUNLAP PLATES 

No. 11 No. 12 No. 13 No. 14 No. 15 No. 16 No. 18 No. 19 No. 20 No. 21 No. 25 No. 27 









14.55 


15.45 






































15.15 


15.25 






























15.5 


15.24 


15 


62 


15.1 


15.2 


15 


38 


14, 


97 


14 


65 


15 


6 


15, 


35 


15, 


6 


14 


66 




15.22: 


15 


42 


15.05 


15.2 


15. 


3 


14 


94 


14 


68: 


15 


51 


15 


24 


15 


49 


14. 


61 


15.6 


15.24 


15. 


35 


15.0 


15.3 


15 


33 


14 


96 


14 


91: 


15 


44 


15, 


29 


15 


48: 


14 


61 


15.5 


15.37 


15. 


55 


14.6 


15.4 


14 


97 


15, 


04 


15, 


17: 


15. 


52 


15, 


34 


14 


58 


14. 


22 


14.85 


15.31 


14. 


85 


15.15 


14.85 


15 


31 


15. 


12 


15. 


47: 


15 


54 


15 


16 


15. 


28 


15 


28 


15.6 


14.88 


15 


19 


14.85 


14.95 


15. 


28 


15. 





15, 


31: 


15. 


50 


14, 


67 


15 


16 


14 


21 


15.55 


15.31 


15. 


44 


14.25 


15.1 
15.0: 


15. 


35 


15 


23 


15 


15 


15. 


46 


14 


94 


15 


34 


14, 


41 


15.2 


15.18 


15. 


30 


14.65 


15.3 


15. 


17 


15, 


28: 


15. 


06 


15. 


24 


15. 


35 


15 


44 


14 


74 


15.35 


14.94 


15. 


50 


14.8 


15.25 


15 


01 


15, 


13 


15, 


31 


15. 


55 


15. 


40 


15. 


40 


14. 


77 


14.85 


14.35 


15. 


61 


15.0 


15.35 


15. 


43 


14 


12 


14, 


97 


15. 


64 


15 


32 


15 


53 


14 


63 


15.4 


15.3 


15. 


52 


15.05 


15.0 


15. 


05 


14. 


4 


14 


56 


15 


51 


15 


32: 


15 


44 


14. 


56 


15. 55 


14.88 


15 


31 


15.1 


15.2 


15. 


22 


15 


34 


15, 


32 


14 


91 


15 


35 


15. 


23 


14 


80 


14.35 


15.46 






14.85 


14.9 
14.9 

15.25 


15. 
15 


08 

1 


14 


51 


15 


34 


14 


77 


14 


82 


15 


49 


14 


38 


15.65 
15,3: 


15.32 


15 


44 


14.95 


15.3 






15 


04 


14, 


88 


15 


35 


15 


34 


15 


48 


14 


12 


15.5 


14.93 


15 


36 


14.9 


15.25 


15 


08 


14 


14 


15 


18 


14, 


92 


15 


35 


15 


40 


14 


4 


15. 55 


15.57 


15. 


63 


14.45 


15.3 


15 





15 


2 


15, 


31 


15, 


28 


15 


33 


14 


81 


14, 


27 


14.8 


15.37: 


14. 


38 




14.6? 


15 


25 


15 


24 


15, 


34 


15 


54 


14 


90 


14 


75 


14, 


59 


15.2 


14.82 


15, 


04 


15.2 


15.3 


15. 


3 


14 


98 


15. 


57: 


15 


53 


15 


25 


15 


69 


14 


66 


15.3 


15.48 


15. 


34 


14.95 


15.35 


15. 


17 


15 


46 


14 


98 


15, 


65 


15 


30 


15. 


39 


14 


64 


15.45 


15.38 


15 


54 


14.95 


15.45 


15. 


15 


15 


21 


14, 


77 


14 


64 


14 


83 


14 


65 


14, 


65 




15.25 


15 


5 


15.0 


14.95 


15 


27 


15 


3 


14 


50 


15 


38 


15 


35 


15 


12 


14 


71 


15.0 


14.37 


15. 


57 


14.95 


14.95 


15. 


29 


14 


35 


14, 


92 


15 


54 


15 


02 


15 


45 


14, 


67 


15. 55 


15.17 


15. 


57 


15.3 


15.25 


14. 


93 


15 


16 


14 


45 


15. 


24 


15, 


33 


14 


75 


14 


58 


14.95 


14.51 


15. 


71 


14.95 


15. 5 


15. 


16 


14. 


99 


14 


97 


14 


41 


14, 


99 


15, 


56 


14. 


66 


15.5 


15.17 


15. 


34 




15. 55 


15. 


08 


15. 


28 


14. 


97 


15. 


48 


15. 


11 


15, 


47 


14, 


51 


14.85 


15.26 


15. 


02 


15.25 


14.75 


15 


16 


14. 


85 


15. 


11 


14, 


88 


14 


98 


15. 


42 


14, 


48 


15.3 


14.26 


15. 


52 


15.4 


14.9 


15. 


21 


13 


82 


15 


56 


15 


56 


14. 


93 


14, 


84 


14 


16 


15.7 


15.38 


15 


56 


15.35 


15.2 


15 


20 


14 


69 


15. 


26 


15, 


72 


15 


33 


15 


58 


14, 


39 


15.2 


15.23 


15. 


64 


15.3 


15.0 


15 


30 


13. 


97 


15 


03 


15. 


72 


14 


92 


15, 


36 


14. 


39 


14.9 


15.67 


15 


51 


14.8 
14.8 


15.35 
14.6 


15, 


25 


14. 


85 


15. 


22 


15. 


28 


15 


2 


15 


06 


14. 


63 


15.6 
15.4 


14.69 


15 


44 


14.9 


14.8 


15 


04 


14. 


87 


15. 


05 


14. 


44 


15. 


45 


14. 


56 


14. 


43 


14.85 


14.70 


15 


4 


14.85 


14.8 


14. 


90 


14, 


73 


15. 


09 


14. 


81 


15. 


07: 


14. 


83 


14. 


15 


14.75 


14.95 


15. 


G 


14.85 


14.9 


15. 


00 


14, 


89 


15, 


10 


15. 


1 


14. 


88 


14. 


95 


13. 


87 


14.75 


14.94 


15 


47 


14.9 


15.25 


14. 


92 


14, 


91 


15. 


10 


15. 


3 


14. 


42 


15. 


09 


14. 





14.95 


15.18 


15 


54 


14.9 
14.95 


15.25 
14.95 


15. 


06 


15, 


08 


15, 


20 


15. 


4 


14. 


65 


15. 


29 


14. 


26 


15.1 


14.80 


15 


49 


14.5 


15.2 


15, 


19 


13, 


85 


15, 


20 


15. 


46 


15. 


38 


14. 


50 


14. 


57 


14.95 


15.02 


15 


62 


14.65 
14.6 


15.25 
15.15 
15.2 


15. 


08 


14 


05 


15, 


26 


15. 


56 


15 


54 


14. 


76 


14. 


54 


15.25 
15.3 



14.80 14.44 14.75 15.3 15.05 15.25 14.95 15.55 15.34 15.55 14.43 15. Si 



16 



Plate 


Julian Day 


8846 


30884 


721 


8851 




771 


8887 


0899 


602 


8891 




647 


8897 




701 


8912 


0900 


604 


8916 




638 


8935 


0901 


632 


8938 




676 


9001 


0932 


604 


9021 


0933 


589 


10098 


1257 


634 


10108 


1258 


625 


10121 


1259 


604 


12043 


1969 


736 


12063 


1970 


698 


12109 


1976. 


641 


12138 


1977 


690 


12276 


2000 


641 


12323 


2004 


652 


12357 


2006 


599 


13326 


2326 


715 


13340 


2328 


739 


13392 


2354 


604 


13415 


2355 


607 


13439 


2356 


605 


13454 


2357. 


604 


13504 


2361 


704 


14506 


2733. 


605 


14530 


2734. 


604 


14578 


2740 


608 


14602 


2741. 


607 


14627 


2742. 


648 


14750 


2770. 


576 


16016 


3068 


668 


16043 


3069 


654 


16167 


3095 


604 


16196 


3096 


609 


17448 


3476. 


602 


17472 


3477 


601 


17504 


3481 


597 


17627 


3505 


572 


18162 


3823 


649 


18273 


3858 


636 


18277 


3859 


590 


18292 


3860 


589 


19147 


4180 


634 


19164 


4181 


607 


19186 


4182 


607 


19191 


4183 


608 


20072 


4538 


633 


20092 


4539 


634 



No. 1 No. 2 No. 3 No. 6 No. 7 No 
15.43 



No. 9 No. 10 



14.62 
14.8 
15. 16 
14.76 
14.62: 



14.55 
14.52 

14.93 
14.93 
15.07 
15.63 
15.31 
14.46 
14.51 
15.54 
15.37 
15.26 
15.29 
14.84 

15.5 

15.28 

14.97 

14.81 

15.49 

14.37 

15.21 

15. 35 

15.54 

15.7 

15.38 

15.26 

15.35 

14.5 

14.3 



15.60 

15.58 
15.50 
15.21 
14.73 
15.38 
15.5 



14.55 15.77 

15.24 15.54 
14.97 

14.93: 14.50 



15.74 
15.21 

15.28 
15.26 
15.55 
15.57 
14.62 
15.52 
15.21 
15.62 
15.51 
15.63 
15.17 
15.15 

15.16 

15.08 

15.37 

15.25 

15.44 

15.35 

15.11 

15.77 

15.52 

15.49 

15.49 

15.0 

15.6 

15.31 

15.68 



15.39 15.16 

14.76 15.4 

14.51 15.04 

15.51 14.98 



15.47 
15.26 
15.22 
15.17 
15.37 
15.25 
14.98 

15.44 
15.03 

15.51 

14.77 
15. 17 

15.42 

15.49 

15.37 

15.38 

15.27 

14.53 

15.82 

15.48 

14.96 

15.32 

15.9 

15.23 

15.5 

15.41 

15. 18 

14.65 

15.42 

15.1 

15.37 

14.91 

15.48 

15.03 

15.45 

14.99 

15. 18 



14. 
15. 



14.87 
14.65 



15.62 
15. 53 



15.44 
15.04 
15.54 
15.18 

15.3 

14.83 



14.95 
14.95 
15.25 
14.95 
15.05 

14.95: 

15.05 
15.05 
15.05 
14.35 

15.05 
15.25 

14.45 
14.75 
15. 15 
14.95 

14.9 

15.25 

15.15 

15.25 

15.2 

14.95 

15.05 

15.15 

14.55 

15.05 

15.3 

15.4 

15.35 

15.5 

15.45 

15.45 

15.25: 

15.25 

14.7 

15.25 
14.9 
15.25 
15.25 

14.85 
14.55 



15.41 
15.41 
15.21 
15.38 
15.55 
15.45 
15.4 

15.44 
15.16 
14.85 
15.23 

15.42 
14.16 

14.26 
14.65 
15.35 
15.41 

14.27 

14.5 

15.65 

15.12 

15.25 

15.36 

15.3 

14.02 
14.48 
15.08 
15.02 
15.48 
15.35 
15.44 
15.25 
15.01 

15.63 

14.1 

15.3 

15.0 

15.26 

15. 17: 
15.64 
15.61 
15.37 

14.00 
14.09 



14.85 

14.99 

15.17 

15.37 

15.59 

14.9 

15.15 

15.01 
15.55 



15.2 
15.34 

14.74 

14.55 

14.6 

15.37 

15.33 

14.96 

15.55 

15.03 

15.77 

15.25 

15.50 

14.75 

15.55 
15.52 
15.7 
15.46 

15.16 

14.57 

15.77 

15. 35 

14.8 

15.7 

14.98 

14.81 

15.35 

15.59 

14.60 
14.82 
15.71 
15.58 

15.37 
15.15 



15.47 
15.26 
15.48 
14.85 
14.58 
15.22 
15.18 

15.42 
14.66 



14.62 
14.72 

14.74 

15.33 

15.1 

14.55 

15.72 

15.47 

15.46 

15.63 

14.9 

15.15 

14.67 

15. 18 

15.35 
14.65 
15.40 
14.70 
14.94 
15.23 
15.52 
14.57 
15.34 
14.79 
15.45 
15.03 
15.47 
15.41 
15.42 



15.55 
15.44 
15.72 
15.55 
15.69 
15.50 
15.50 

15.42 
15.63 



15.45 14.86 15.29 



15.16 
15.15 

14.96 
14.75 
15.40 
15.09 
15.23 
15.60 
15.54 
15.46 
14.84 
14.86 
14.51 
15.41 

15.57 

15.14 

15.53 

15.6 

15.28 

14.48 

15.48 

15.17 

15.78 

15.28 

15.37 

15.11 

15.23 

15.65 

15.50 



15.35 15.34 

15.36 15.37 
15.49 

15.25 14.82 



15.4 
14.85 



14.59 
14.65 



17 



No. 11 


No. 12 


No. 


13 


No. 14 


No. 


15 


No. 


16 


No. 


18 


No. 


19 


No. 


20 


No. 21 


No. 25 


No. 27 


14.21 


14.98 


14. 


85 


15.55 


15. 


11 


15. 


58 


15. 


05 


15. 


66 


15. 


39 


15.66 


14.21 


15.3 


14.58 


15.22 


14. 


8 


15.3 


14. 


94 


15. 


18 


15. 





15. 


48 


15. 


38 


15.35 


14.05 


15.4 


14.2 


14.58 


15. 





14.5 


15. 


10 


15. 


22 


14. 


97 


15. 


58 


14. 


55 


15.41 


14.56 


15.25 


14.3 


14.44 


14. 


85 


14.8 


15. 


10 


15. 


13 


15. 


04 


15. 


65 


14. 


58 


15.40 


14.48 


15. 15 


14.66 


14.94 


15. 


2 


15.0 


15. 


39 


15. 


41 


15. 


25 


15. 


83 


14. 


82 


15.62 


15.62 


15.3 


15.06: 


14.75 


14. 


8 


14.65 


15. 


05 


14. 


68 


15. 





15. 


71 


15. 


3 


14.86 


14.42 




15.41 


15.04 


14. 


65 


14.8 


15. 


12 


14. 


79 


15. 


26 


15. 


54 


15. 


3 


14.95 


14.67 


15.2 


15.35 


15.45 


14. 


95 


15.25 


15. 


21 


15. 


42 


15. 


32 


15. 


65 


15. 


35 


15.67 


14.67 


15. 5 


15.29 


15.86 


14. 


95 


15.6 


14. 


68 


15. 


15 


15. 


17 


15. 


82 


14. 


67 


14.55 


14.29 


15.3 


14.1 




14. 


95 


15.5 






14. 


20 
















13.97 


15.6 


15.45 


15.53 


15. 


2 




15. 


12 


14. 


89 


14. 


56 


15. 


19 


15. 


12 


15.27 


14.52 


15.25 


14.71 


15.66 


15. 


25 


15.5 


14. 


89 


15 


07 


15 


16 


15. 


48 


15. 


45 


15.32 


14.56 


15.5 


15.35 


14.30 


15. 


25 


14.6 
14.4 


15. 


06 


13 


78 


15. 


31 


15. 


6 


15. 


39 


15. 58 


14.45 


15.5 


15.24 


15.63 


14 


7 


15.2 


15 


17 


15 


06 


15 


27 


15 


01 


14 


77 


14.79 


14.52 


15.2 


14.7 


14.18 


15 





15.4 


15. 


4 


14 


81 


15 


52 


15 


63 


15. 


49 


15.59 


14.45 


15.45 


15.44 


14.37 


15 


25 


15. 5 


15 


31 


15 


25 


15 


11 


15 


16 


15. 


31 


15.46 


14.7 


15.3 


15.30 


15.7 


15 


2 


15.4 


15 


4 


14 


40 


15 


64 


15 


75 


14 


62 


15.20 


14.53 


15. 5 




15.81 


15 


4 


15.5 


14 


95 


14 


32: 


14 


32: 


15 


55 






15.25 


14.43 


15.15 


15.26 


15.02 


14. 


85 


15.0 


14. 


90 


14 


38 


15 


24 


14 


48 


15 


27 


15.50 


14.35 


15.6 


14.95 


15.51 


15 


25 


14.95 


14. 


96 


14 


75 


14 


96 


15 


54 


15 


41 


14.61 


14.35 


15.45 


15.59 


15.74 


15 


1 


14.45 


15 


33 


14. 


9 


15 


05 


15 


63 


15 


1 


15.82 


14.48 


15.6 


15.27 


14.17 


15 


4 


14.85 


15 


36 


15 


16 


14 


64 


15 


87 


15 


00 


15.42 


14.48 


14.9 


14.53 


14.86 


15 


3 


14.8 


15 


1 


14 


77 


14 


93 


15 


40 


15 


51 


14.59 


14.28 


14.55 


15.30 


15.21 


15 


3 


14.95 


15 


35 


15 


22 


15 


1 


15 


61 


14 


92 


15.51 


14.29 


15.0 


15.35 


14.40 


15 

14 


3 
95 


15.5 
14.4 


15 


02 


14 


67 


14 


99 


15 


56 


15 


13 


15.40 


14.64 


15. 55 
15.6 


15.48 


15.38 


14 


95 


14.6 


14 


92 


13 


97 


15 


29 


14 


63 


15 


59 


14.63 


13.84 


15.15 


15.39 


14.83 


14 


55 


15.2 


14 


84 


14 


69 


15 


23 


15 


56 


15 


26 


15.02 


13.75 


15.55 


14.72 


15.42 


14 


9 


15.25 


15 


01 


15 


25 


15 


60 


15 


86 


15 


12 


15. 56 


14.33 


15.5 


15.33 


15.7 


14 


75 


15.25 


14 


79 


14 


71 


14 


49 


14 


60 


14 


66 


15.17 


13.57 


15.6 


15.36 


15.12 


15 


15 


15.2 


14 


87 


15 


20 


14 


98 


15 


52 


15 


49 


15.46 


14.19 


15.15 


14.17 


15.50 


15 


15 


15.5 


14. 


93 


15 


01 


15 


35 


15 


60 


15 


30 


15.24 


14.51 


14.55 


15.26 


15.62 


14 


85 


15.45 


14 


79 


14 


58 


15 


44 


15 


78 


15 


28 


15.39 


14.34 


14.75 


14.8 


14.93 






14.8 


14 


9 


14 


73 


15 


68 


14 


75 


14 


74 


15, 65 


14.65 


15.25 


15.35 


15.18 
15.46 


15 


25 


14.9 

14.85 


14 
15 


96 
2 


14 


01 


15 


38 


15 
15 


09 
60 


15 


34 


15.48 
15.51 


14.51 
14.06 


15.6 


15.14 


15.67 


14 


9 


14.75 


15 


31 


14 


76 


15 


59 


15 


43 


15 


50 


15.30 


14. 1 


15.6 


14.34 


15.46 






15.1? 


14 


91 


14 


76 


14 


65 


15 


27 


15 


25 


15.07 


14. 18 




14.94 


15.58 






15.25 


15 


32 


15 


14 


14 


96 


15 


5 


15 


43 


15.60 


14.40 


14.6 


14.07 


15.59 






15. 5 


14 


85 


14 


7 


14 


75 


15 


17 


15 


24 


15.41 


14.07 




15.26 


15.70 


15 


3 


15.3 


15 


01 


14 


75 


14 


92 


15 


74 


14 


47 


15.07 


14.42 


15.6 


14.2 


15.62 






15.4 


15 


44 


15 


06 


14 


83 


15 


57 


15 


09 


15.44 


14.68 




14.32 


14.32 


14 


9 


15.35 


14 


98 


15 


31 


15 


57 


15 


63 


15 


25 


15.42 


14.73 


15.5 


15.49 


14.69 


15 


05 


15. 55 


15 


16 


15 


11 


15 


59 


15 


78 


14 


7 


15.09 


14.58 


15.6 


15.31 


15, 13 


14 


9 


15.2 
15.2 

14.85 


15. 


04 


14. 


91 


15. 


27 


14. 


48 


15. 


35 


15.62 


14.33 


15. 5 


15.39 


15.51 


14 


7 


14. 


86 


14 


89 


14 


95 


15. 


59 


15. 


11 


15.35 


14.33 




15.33 


15.59 


14 


9 


15.2 


14. 


88 


14 


30 


15. 


11 


15. 


67 


15. 


11 


14.69 


14.33 


15.7 



18 



Plate 


Julian 


Day 


20110 


34540 


613 


20227 


4572 


602 


20240 


4573 


635 


20255 


4574 


602 


20274 


4575 


603 


21394 


4929 


623 


22336 


5273 


612 


22356 


5274 


609 


22373 


5275 


610 


22470 


5307 


600 


22491 


5308. 


599 


22514 


5309 


600 


22538 


5310 


600 


23203 


5658 


601 


23215 


5661 


602 


23293 


5685 


588 


23313 


5687 


592 


23327 


5688 


590 


24782 


6752 


607 


24803 


6753 


602 


25182 


7113 


610 


25209 


7115 


636 


25231 


7116 


640 


26824 


8198 


614 


26845 


8199 


629 


27544 


8584 


628 


27551 


8586 


605 


29082 


9262 


772 


29083 




779 


29084 




785 


29087 


9265 


585 


29092 




620 


29097 




680 


29098 




684 


29099 




772 


29103 




816 


29104 




819 


29106 




847 


29138 


9270 


772 


29139 




776 


29141 




798 


29142 




803 


29148 


9271 


615 


29149 




.619 


29151 




.647 


29152 




.651 


29155 




697 


29156 




.701 


29158 




.722 


29159 




.725 


29164 




771 


29165 




776 


29169 




.817 


29170 




820 



No. 1 No. 2 No. 3 No. 6 No. 7 No. 



No. 9 No. 10 



14.33 


15.49 


15.37 


15.25 


14.20 


14.67 


15.44 


15.53 


15.09 


14.96 


14.81 


14.6 


15.05 


15.49 


15.32 


14.94 


15.1 


14.85 


15.3 


14.65 


15.15 


15.37 


15.38 


14.51 


14.5 


15.6 


15.25 


15.3 


16.0 


15.69 


15.17: 


15.17 


14.43 


15.58 


14.7 


15.25 


15.48 


14.76 


15.46 


15.26 


15.33 


15.80 


15.38 




15.61 


14.82 


14.74 


15.55 


15.44 


14.82 


14.69 


14.9 


14.69 


15.6 


15.11 


14.72 


15.51 


14.61 


15.42 


14.85 


15.29 


15.53 


15.48 


14.46 


15.16 


15.86 


14.91 


14.5 


15.15 


15.69 


14.85 


15.22 


15.10 


15.62 


15.38 


15.0 


15.13 


14.91 


14.81 


14.98 


15.5 


15.65 


15.24 


14.7 


15.07 


14.8 


15.26 


14.56 


15.54 


15.7 


14.92 


14.95 


15.39 


15.57 


15.55 


15.36 


15.49 


15.52 
15.56 


15.38 


15.0 
15.0 


15.31 


15.6 


14.99 


15.54 


15.27 


14.93 


15.5 


15.05 


15.12 




15.56 


14.98 


15.08 


15.08 


15.26 


14.65 


15.44 


14.92 


15.44 


15.6 


14.63 


15.85 


15.30 


15.4 


15.06 


15.52 


15.28 


14.81 


14.55 


15.52 


15.31 


15.25 


14.65 


15.55 


14.72 


14.76 


14.87 


15.48 


15.01 


14.8 


14.46 


15.68 


15.31 


14.85 


14.55 


15.63 


15.16 


14.7 


14.59 


15.52 


14.78 


14.02 


14.62 


15.57 


15.4 


14.95 


14.92 


15.52 


14.61 


15.52 


14.23 


15.43 


14.83 


15.1 


15.15 


14.91 


14.75 


15.29 


15.10 


15.30 


15.34 




15.23 


14.78 


15.15 


15.02 


15.37 


14.96 


15.3 


15.2 


15.44 


15.43 


15.33 


15. 11 


15.29 


15.35 


15.02 






15.5 


14.70 


14.53 


15.28 


15.38 


15.35 


15.1 


15.25 


15.42 


15.43 


15.37 


14.92 


15.53 


15.15 


15.05 


15.47 


14.82 


15.44 


15.1 


14.42 


14.72 


15.28 




14.82 


14.75 


14.85 


15.48 


14.38 


14.91 


15.41 


15.25 
14.75 


15.15 


14.49 


14.95 


15.61 



15.15 15.7 15.2 



13.95? 15.27 15.05 14. 



15.27 


15.60 


15.31 




14.44? 


15.41 


15.22 


14.92 


15.4 


15.47 


15.31 


15.05 


15.31 


15.61 


15.28 


14.95 


15.65 


15.63 


15.43 


14.9 


15.24 


15.38 


15.31 


15.11 


15.53 


15.34 


15.50 


14.95 


15.47 


15.65 


15.39 


15.30 


15.10 


15.35 


15.30 


15.05 


15.2 


15.49 


15.27 


15.44 


15.22 


15.35 


15.31 




15.35 


15.42 


15.28 


15.58 


15.03 


15.62 


14.93 


15.25 


15.36 


15.43 


15.27 


15.45 


15.28 


15.6 


14.96 




15.26 


15.5 


15.31 


15.56 


15.11 


15.56 


15. 11 


14.95 


14.71 


14.83 


15.32 


15.00 


15.02 


15.66 


15.16 


14.8 


14.84 


14.90 


15.5 


14.91 


14.43 


15.27 


15.12 


14.6 


14.82 


14.97 


15.38 


15.00 


14.49 


15.07 


15.27 


14.55 


14.88 


14.98 


15.49 


15.00 


14.33 


14.79 


15.15 


14.65 


15.12 


15.06 


14.92 


14.92 


14.60 


14.60 


15.44 


14.6 


15.05 


15.22 


14.88 


15.20 


14.72 


14.72 


15.34 


14.9 


15.16 


15.3 


14.91 


15.18 


14.82 


14.81 


15.38 


14.65 


15.22 


15.24 


14.72 


15.44 


15.08 


15.14 


15.34 


15.1 
14.9 


15.48 


15.41 


14.51 


15.48 


15.10 


15.23 


15.27 


14.95 


15.48 


15.5 


14.69 


15.36 


15.07 


15.32 


15.35 




15.37 


15.45 


14.76 


15.45 



19 



No. 11 No. 12 No. 13 No. 14 No. 15 No. 16 No. 18 No. 19 No. 20 No. 21 No. 25 No. 27 



55 



15.5 

14.69 

15.2 

15.7 

15.79 

15.69 

15.63 

14.32 

14.87 

15.63 

15.64 

15.9 

14.23 

15.33 

15.77 

14.3 

14.82 

14.61 

15.07 

14.73 

15.27 

15.57 

15.48 

14.81 

14.82 

15.43 



15.25 

14.95 

14.95 

14.95 

14.9 

14.65 

14.95 

15.15 

14.95 

15.2 

15.15 
15.15 

15.2 

14.8 

14.85 

14.9 

14.95 

15.15 

15.0 

14.95 

14.85 

15.4 

14.8 



15.25 

14.85 

14.75 

14.7 

14.85 

14.5 

14.65 

14.65 

14.55 

15.5 

15.2 

15.6 

15.4 

14.95 

15.3 

15.5 

15.65 

15.6 

15.0 

15.0 

14.65 

14.7 

14.8 

14.8 

14.9 

15.35 

15.2 



14.95 

15.18 

15.06 

15.28 

15.08 

14.68 

15.31 

15.25 

15.28 

15.24 

15.2 

15.2 

15.14 

15.58 

15.01 

15.02 

15.21 

15.04 

14.95 

15.15 

15.1 

15.08 

14.81 

14.83 

15.17 

15.15 



14.84 
14.20 
15.03 
14.49 
15.11 
14.49 
15.20 
14.14 
14.72 
13.88 
14.81 
14.16 
15.12 

15.22 
14.92 
14.75 
14.49 
14.13 
14.77 
15.23 
15.26 
14.84 
13.75 
14.76 
14.26 
14.41 



15.30 

15. 11 

15.03 

15.55 

14.8 

14.83 

14.68 

15.05 

15.09 

15.15 

15.24 

15.39 

15.49 

15.09 
15.39 
14.81 
15.07 
15.24 
14.29 
14.68 
15.18 
15.18 
15.06 
14.96 
15.23 
15.45 



15.80 
15.52 
14.37 
15.00 
15.15 
15.59 
15.45 
15.76 
15.70 
15.65 
15.49 
15.00 
14.51 



14.97 

15.0 

15.38 

15.16 

15.41 

15.36 

15.45 

15.58 

15.51 

14.55 

15.21 

15.33 



14.53 

15.5 

14.93 

15.16 
15.09 
15.53 
14.98 
15.20 
15.23 
14.59 
15.50 
15.19 

14.89 
15.34 
15.59 
15.27 
15.09 
14.99 
15.34 
14.80 
15.55 
15.49 
15.35 
14.97 
15.5 



15.57 
15.33 
15.17 
15.78 
15.46 
15.52 
15.32 
14.90 
15.46 
15.55 
15.20 
14.95 
15.41 

15.66 

15.43 

15.55 

15.4 

15.16 

14.85 

15.32 

15.48 

15.21 

14.60 

15.38 

15.02 

15.34 



14.47 

14.37 

14.48 

14.78 

14.51 

14.39 

14.58 

14.48 

14.21 

14.59 

14.5 

14.5 

14.37 

14.24 

14.51 

14.26 

14.06 

14.06 

14.48 

14.55 

14.42 

14.41 

14.89: 

14.42 

14.35 

14.36 

14.45 



15.8 

15.6 

14.6 

14.85 

15.15 

15.4 
15.6 
15.5 
15.6 

15.6 
14.95 

15.25 

15.3 

15.4 



15. 
14. 



15.6 
15.25 

15.6 

14.95 



14.48 
14.45 



15.12 



15.25 



15.5 
14.7 
15.0 
15.35 



14.8 
14.9 



14.58 
14.65 



15.15: 
15.29 



14.88 
14.89 



15.05 
15.27 



15.1 
15.17 



14.42 
14.31 



15.35 14.88 15.38 15.34 15.13 14.65 14.54 



14.8 



15.43: 

15.60 

15.72 

15.73 

14.87 

14.98 

15.14 

15.05 

14.95 

14.72 

14.40 

14.36 

14.97 

14.76 

14.9 

14.89 

15.3 

15.33 
15.32 



15.15 
15.25 
15.3 

14.8 

14.9 
14.9 
15.2 
15.15 



14. 
14. 



14.55 

14.5 

14.85 

14.8 

14.95 

14.85 

14.85 



15.6 

15.65 

15.5 

15.6 

15.55 

15.5 

15.3 

15.25 

15.65 

15.45 

15.65 

15.55 

15.4 

15.55 

15.5 

15.55 

15.35 

15.25 

14.4 

14.35 



14.84 

14.93 

14.93 

15.07 

15.09 

15.0 

14.92 

14.88 

14.97 

15.15 

15.06 

15.25 

15.19 

15.4 

15.25 

15.27 

15.14 

14.99 
14,95 



15.22 
15.22 
15.35 
15.13 

14.82 



15. 
14. 
15. 
15. 



05 

88 
18 
11 



15.34 
15.09 
15.31 
14.03 
14.33 
13.90 
13.98 
13.93 

14.40 
14.37 



15.03: 

14.77 

14.65 

14.97 

15.34 

15.17 

15.22 

15.14 

15.22 

15.36 



15. 
15. 



12 

23 



14.97 
15.19 
15.28 
15.42 
14.92 

14.96 
14.81 



15.45 
15.67 
15.47 
15.78 
14.93 
14.89 
15.05 
14.98 
14.91 
14.83 
14.39 
14.47 
14.63 
14.72 
14.93 
14.81 
15.2 



15.32 

15.37 

15.6 

15.17 

14.48 

14.46 

14.76 

14.55 

15.25 

15.39 

15.26 

15.31 

15.55 

15.35 

15.22 

15.58 

15.4 



15.36 15.41 
15.25 15.32 



15.01 
15. 17 
15.15 
15.29 
15.28 
15.22 
15.31 
15.31 
15.22 
15.51 
14.98 
14.88 
14.31 
14.45 
14.59 
14.50 
14.83 

14.99 

14.98 



14.05 
14.25 
14.18 
14.30 
14.25 
14.22 
13.97 
13.92 
14.63 
14.67 
14.57 
14.62 
14.41 
14.52 
14.47 
14.66 
14.39 

14.01 
14.02 



15.5 

15.25? 

15.6 

14.8 

14.85 

14.8 

15.5 

15.5 

15.35 

15.4 

14.65 

14.55 

14.7 

14.6 

15.2 

15.3 



20 



Julian Day No. 28 No. 29 No. 30 No. 31 No. 32 No. 33 No. 34 No. 35 No. 36 

28308.736 15.3? 15.25 

8309.651 15.4 14.9 

.661 15.33 15.6 15.6 15.1 15.6 15.5 15.20 15.13 14.85 

.670 15.25 15.5 15.43 14.99 15.49 15.3 15.05 15.10 14.95 

.677 15.35 15.42 15.09 15.43 14.85? 15.10 14.9 

.796 15.27 15.4 14.89 15.09 15.36 15.0 14.80 14.70 14.95 

8365.608 15.1 15.53 15.34 14.96 15.57 14.9 15.20 14.75 15.05 

8366.608 14.62 15.65 14.83 15.18 14.34 15.0 15.1 14.98 15.25 
8399.596 15.56 15.52 15.44 15.00 14.7 14.4 14.8 15.17 14.9 
8688.640 14.9: 

8689.642 

8692.632 15.29 15.3 15.35 14.87 14.97 15.1 14.65 15.10 14.7 

8693.730 15.30 15.42 15.37 15.29 15.48 15.3 14.95 14.77 14.7 

8696.631 15.47 15.6 15.35 15.15 15.40 15.2 14.55 15.18 15.15 

8715.638 

9071.660 15.02 15.47 15.33 14.92 14.8 15.05 15.08 14.7 

9072.698 15.02 15.42 15.35 15.32 15.38 15.1 14.9 14.99 14.9 

9073.605 15.50 15.75 15.21 15.19 15.25 14.9 15.5 14.89 14.75? 

9076.603 15.4 
9077.600 14.4 

9078.600 14.4 15.1 14.55: 

9079.602 15.27 14.64 14.69 15.10 15.32 14.7 14.95: 15.30 

9786.609 15.39 15.19 15.06 15.42 15.46 15.75 15.35 15.12 14.9 
9787.608 15.39 15.55 15.53 15.17 14.61 15.55 15.1 15.20 15.25 

9813.610 15.26 14.96 15.46 15.19 15.57 15.25 14.66 15.1 

9814.612 14.87 15.20 15.25 15.49 14.65 15.5 15.35 14.94 15.25 

9815.613 15.11 15.34 15.13 15.23 15.4 15.1 15.23 14.65 

9816.611 15.42 15.52 15.38 15.19 15.44 15.15 15.2 15.15 14.95 
30171.617 15.36 14.78 14.97 15.24 15.30 15.4 14.95 15.22 14.7 

0172.615 15.23 15.26 15.53 15.43 14.75 15.6 15.13 14.9 

0519.606 14.88 15.33 15.31 14.30 15.55 15.5 15.13 15.3 
0520.606 15.33 15.26 15.15 15.6 15.35 14.85 15.25 
0550.608 14.95 15.28 14.90 14.91 15.35 15.5 14.64 14.85 

0553.604 15.25 14.87 14.98 14.90 15.12 15.25 15.5 14.71 15.35 

0554.614 15.36 15.66 15.56 15.56 15.45 15.2 15.5 14.50 14.7? 
0555.629 15.59 15.70 15.52 14.96 15.57 15.35 14.96 
0556.620 15.00 15.43 15.24 15.03 14.92 15.25 15.45 15.03 15.55 
0586.572 15.19 15.04 15.39 14.81 15.26 14.55 15.25 14.75 15.3 

0880.592 15.05 14.65 15.2: 
.623 15.37 15.70 15.37 14.85 15.50 15.3 14.8 14.66 15.05 
.659 14.61 15.49 15.33 15.1 15.41 15.05 14.8 14.60 15.15? 
.690 14.51 15.70 15.50 15.3 15.58 15.4 14.9 14.70 15.05 
.730 14.79 15.50 15.50 15.39 15.31 15.3 15.1 14.81 15.0 
.760 14.97 15.37 15.46 15.44 14.22 15.5 14.95 15.05 15,0: 

0880.788 

0883.593 15.05 

.630 15.28 15.22 15.42 14.95 15.10 15.05 15.2 15.11 15.1 

.664 15.50 15.45 15.42 15.14 15.39 15.40 15.2 15.00 14.9 

0884.622 15.30 

.680 15.32 15.61 15.25 15.42 15.60 15.55 14.95 14.70 15.0 



21 



No. 38 No. 39 No. 40 No. 41 No. 42 No. 43 No. 44 No. 45 No. 47 No. 52 No. 55 



14.75 














15.1 








14.85 








12.4 






14.6 








14.85 


15.00 


15.17 


15.13 


12.4 


15.08 


14.92 


14.65 


14.96 


14.46 


15.34 


14.85 


15.02 


15.21 


15.22 


12.4 


15.15 


14.91 


14.7 


14.99 


14.37 


15.23 


14.9 


15.15 


15.27 


15.26 


12.3 


15.20 


14.71 


14.7 


14.70 


14.29 


15.20 


15.05 


15.26 


15.11 


15.60 


12.4 


15.08 


14.82 


14.95 


14.28 


14.69 


15.02 


14.6 


14.90 


15.37 


15.54 


10.7 


15.10 


15.09 


15.2 


15.15 


15.12 


15.36 


14.9 


15.61 


15.07 


15.60 


10.7 


15.39 


15.15 


15.25 


15.0 


15.12 


15.35 


15.05 


15.65 


15.21 


15.35 


11.8 
11.9 
12.1 


15.31 


15.25 


14.4 


15.40 


15.02 


15.15 


14.9 


15.17 


15.09 


14.87 


12.6 


15.25 


15.15 


14.7 


15.11 


15.04 


15.00 


15.15 


15.02 


15.35 


15.45 


12.4 


15.21 


14.88 


14.55 


15.20 


15.05 


15.05 


15.25 


14.8 


15. 13 


15.35 


12.1 
12.4 


15.35 


14.97 


15.2 


15.33 


15.08 


14.95 


14.4 


15.42 


15.33 


15.49 


11.9 


15.33 


15.10 


15.15 


15.17 


14.85 


15.01 


14.9 


15.42 


15.07 


14.51 


12.1 


15.17 


15.00 


15.25 


15.40 


15.15 


15.30 


14.6 


14.88 


15.20 


15.44 


12.2 


15.43 
15.20 


15.07 
15.02 


14.65 

14,7 


14.94 


14.81 


14.92 


15.05 


14.95 


15.27 


14.9 


12.6 






15.5 


15.14 


14.83 


15.06 


15.15 


15.39 


15.31 


15.25 


11.6 


15.20 


15.11 


15.15 


14.91 


14.97 


14.95 


15.4 


15.18 


15.37 


15.35 


11.7 


15.54 


15.10 


15.3 


14.64 


15.04 


14.94 


15.4 


15.34 


15.28 


15.53 


11.9 


14.98 


15.11 


14.9 


15.00 


15.18 


15.02 


15.15 


14.82 


15.04 


15.63 


11.7 


15.49 


15.17 


15.25 


14.76 


15.28 


15.09 


15.15 


15.43 


15.01 


15.60 


11.8 


15.15 


15.13 


14.95 


14.41 


15.40 


15.10 


15.15 


15.32 


15.02 


15.48 


11.7 


15.46 


15.12 


14.75 


15.37 


15.28 


15.06 


14.6 


15.04 


14.95 


15.28 


11.5 


15.42 


14.93 


15.1 


15.50 


15. 15 


15.31 


14.9 


15.35 


14.93 


15.35 


11.7 


15.40 


14.85 


14.9 


15.20 


15.16 


15.30 


15.35 


14.25 


15.28 


15.55 


12.6 














14.15 


15.52 


15.24 


15.57 


12.7 


15.53 


15.24 


14.75 


15.21 


14.37 


15.10 


14.8 


15.38 


15.06 


14.37 


11.7 


15.24 


15.57 


14.95 


14.99 


14.41 


15.25 


14.5 


15.37 


15.34 


15.03 




15.38 


15.06 


14.65 


15.20 


14.33 


14.88 


14.9 


15.47 


14.78 


15.02 


11.7 


15.18 


14.90 


14.7 


14.90 


14.35 


14.78 


15.4 


14.76 


14.88 


15.27 




15.60 


14.40 


15.25 


14.80? 


13.50 


14.95 


15.4 


15.65 


14.95 


15.28 


11.3 


14.79 


14.54 


15.2 


14.15 


13.75 


14.98 


14.85 


15.42 


15.30 


15.54 


11.9 


15.49 


14.62 


14.65 


14.64 


14.20 


14.99 


14.6 










15.46 


14.97 


15.25 


15.34 


15.16 


15.05 


15.0 


15.55 


14.97 


15.59 


12.6 






15.0 








15.1 


14.85 


15.10 


15.47 


12.4 


15.29 


14.76 


14.95 


14.90 


14.78 


15.05 


15.05 


14.31 


15.25 


15.54 


12.4 


15.17 


14.61 


14.95 


14.69 


13.95 


15. 16 


15.15 


14.50 


15.31 


15.50 


12.4 


15.32 


14.70 


15.15 


14.95 


13.98 


15.36 


15.3 


14.77 


15.32 


15.58 


12.4 


15.25 


15.39 


14.9 


14.93 


14.26 


15.34 










12.4 


15.40 


15.05 


14.95 


15.21 


14.55 


15.30 










12.4 






14.8 








15.35 


14.21 


15.25 


15.55 


12.6 


15.49 


14.66 


14.95 


15.17 


14.90 


15.24 


15.15 


14.39 


15.15 


15.62 


12.5 
12.2 


15.50 


14.80 


14.95 
14.9 


15.37 


14.50 


15.35 


15.15 


15.60 


14.85 


15.58 


12.2 


15.38 


14.85 


14.15 


15.23 


14.17 


15.35 



22 



Julian Day 


No. 28 


No. 29 


No. 30 


No. 31 


No. 32 


No. 33 


No. 34 


No. 35 No. 36 


30884.721 


15.53 


15.05 


15.43 


15.38 


15.61 


15.40 


14.8 


14.94 


14.9 


.771 


15.44 


15.52 


15.38 


14.90 


15.41 


15.30 


15.1 


15.06 


14.9 


0899.602 


15,45 


15.45 


15.39 


15.19 


14.78 


15.20 




15.12 


14.85 


.647 


15.50 


15.67 


15.48 


15.31 


15.14 


15.15 


15.35 


15.14 


14.7 


.701 


14.65 


15.42 


15.58 


15. 5 


15.46 


15.40 


15.35 


14.84 


14.8 


0900.604 


15.37 




14.91 


15.41 


15. 20 


15.20 


15.2 


14.90 


15.2: 


.638 


15.4 


15.21 


15.31 


15.41 


15.41 




14.95 


14.77 




0901.632 










15.60 










.676 


15.32 


15.43 


15.08 


15.15 


15.60 


15.30 


14.7 


14.87 


14.9 


0932.604 


15.17 


15.64 


15.12 


14.75 


15.04 


14.85 


15.3 


14.78 


15.05 


0933.589 




14.90 








14.85 


15.4 


14.80 


15.25 


1257.634 


14.40 


15.60 


14.75 


15.31 


15.06 


15.2 


15.25 


14.55 


14.95 


1259. 6C4 


15.25 


15.14 


15.25 


14.77 


15.5 


14.7 


14.8 


15.15 


15.3 


1969.736 


14.98 


15.28 


15.49 


15.34 




15.15 


14.4 


14.90 


15.3 


1970.698 




















1976.641 


15.47 


15.48 


15. 11 


15.34 


15.55 


14.45 


14.8 


14.65 


15.35 


1977.690 


15.67 


15.19 


14.55 


14.85 


14.82 


14.55 


14.6 


14.90 


15.3 


2000.641 


14.56 


15.56 


15.46 


15.16 


15.23 


15.25 


15.5 


14.99 


14.85 


2004.652 


15.83 


15.70 


15.48 


15.43 


14.36 


15.25 


15.4 


14.70 


15.3 


2006.599 


14.66 


14.99 


15.41 


14.87 


15.17 






14.01 


15.3 


2326.715 


15.38 


14.79 


15.48 


14.85 


15.60 


14.9 


15.25 


14.95 


15.2 


2328.739 


14.98 


15.54 


15.6 


15.06 


14.18 


15.15 


14.85 


14.90 


15.35 


2354.604 


15.8 


15.52 


15.57 


15.17 


15.60 


15.4 


15.6 


14.90 


14.65 


2355.607 


15.46 


14.67 


15.34 


15.17 


15.70 


15.4 


15.15 


15.22 


15.6 


2356.605 


15.16 


15.52 


15.28 


15.18 


15.27 


15.3 


14.55 


14.92 


14.95 


2357.604 


15.2 


15.26 


15.37 


14.88 


14.37 


15.45 


15.3 


14.69 


15.3 


2361.704 


15.4 


15.61 


15.46 


15.37 


14.19 


15.25 


14.6 


14.90 


15.15 


2733.605 












15.5 


15.6 




15.6 


2734.604 


15.16 


15.80 


14.96 


14.82 


15.53 


15.4 


15.6 


14.53 


15.15 


2740.608 


15.13 


14.89 


15.03 


14.84 


15.45 


15.35 


15.4 


14.83 


15.2 


2741.607 


15.16 


15.20 


14.86 


15.44 


15.84 


15.4 


15.5 


14.75 


15.35 


2742.648 


14.75 


15.73 


15.60 


14.86 


14.68 


15.4 


15.5 


14.66 


15.2 


2770.576 


15.39 


15.43 


14.96 


15.21 


14.80 


14.95 


15.4 


14.63 


15.3 


3068.668 


15.35 


15.55 


15.30 


15.27 


15.26 


15.4 


15.1 


14.73 


15.5 


3069.654 


15.12 


15.22 


14.64 


15.25 


15.53 


15.4 




14.87 


14.85 


3095.604 


14.68 


16.02 


15.74 




15.10 


15.3 


15.45 


15.35 


15.4 


3096.609 


15.45 


15.51 


15.32 


15.31 


15.25 


15.2 


15.35 


14.70 


14.7 


3476.602 




15.36 


15.13 


15.44 


15.36 




15.45 


14.54 




3477.601 


15.34 


15.68 


15.48 


15.01 


15.80 




15.35 


14.69 


14.95 


3481.597 




15.57 


15.28 


14.98 


15.12 


14.85 


15.2 


14.43 




3505.572 


15.43 


15.6 


14.96 


14.81 


15.36 


14.85 


15.25 


14.85 


15.25 


3823.649 


15.09 


15.16 


15.09 


14.98 


15.57 


15.15 


15.25 


14.16 




3858.636 


15.40 


15.76 


15.36 


15.46 


15.03 


14.45 


15.35 


15.12 


14.95 


3860.589 


15.15 


14.75 


15.45 


14.89 


14.96 


15.55 


15.35 


14.72 




4180.634 


15. 55 


14.68 


14.98 


14.95 


15.29 


14.6 


15.35 


15.05 


14.85 


4181.607 


15.59 


14.95 


15.67 


15.01 


15.64 


14.45 


15.25 


15.31 


15.25 


4182.607 


15.27 


15.41 


15.27 


15.30 


15. 55 


14.35 


15.1 


15.00 


14.95 


4538.633 


14.49 


14.76 


15.47 


15.02 


15.29 


14.5 


15.55 


14.59 




4539.634 


15.49 


15.28 


15.29 


15.04 


15.67 


14.45 


15.45 


14.57 


15.3 



23 



14.2 


15.57 


15.07 


15.60 


12.2 


15.43 


15.18 


14.65 


15.45 


14. 


34 


15.34 


14.2 


15.19 


15.11 


14.76 




15.41 


15.20 


14.7 


15.05 


14. 


63 


15.02 


15.25 


14.70 


14.99 


15.38 


12.2 


14.97 


15.05 


14.8 


15.00 


15. 


17 


14.85 


15.15 


14.85 


14.95 


15.41 


12.1 


14.92 


15.15 


14.95 


15.19 


15. 


19 


14.98 


15.25 


15.11 


15.22 


15.66 


12.1 


15.04 


14.87 


15.25 


15.29 


15. 


25 


15.24 


15.45 


15.31 


15.05 


15.52 


12.2 


15.33 


14.99 


15.3? 


15.14 


15. 


19 


14.84 




15.55: 


15.25 


15.44 




15.46 


15.21 


14.95 


15.14 


15. 


25 


15.06 


14.2 


15.52 


15.27 


15. 52 




15.15 


15.19 


15.35 


15.07 


15. 


45 


15.36 


15.25 


14.78 


14.77 


15.80 


12.9: 


14.81 


14.94 


15.25 


15.10 


14. 


94 


15.34 


15.25 








12.8: 




14.95 


15.2 


14.82 


15. 


07 




15.4 


15.00 


15.13 


14.78 


11.7 


15.25 


14.92 


15.25 


15.10 


15. 


02 


15.28 


15.3 


15.29 


15.29 


14.91 


12.0 


15.42 


15.10 


14.65 


15.10 


15. 


02 


15.20 


15.05 


15. 59 


15.08 


15. 56 


11.3 
11.4 


15.47 


14.44 


15.1 


14.12 


14. 


47 


15.23 


14.2 


15.48 


14.86 


15.51 


11.9 


15.28 


14.79 


15.3 


14.77 


13. 


84 


15.24 


14.65 


15.33 


15.30 


15.44 


12.0 


15.24 


14.92 


15.3 


15.35 


14. 


34 


14.93 


14.25 


15.75 


15.27 


15.51 


11.6 


15.42 


14.84 


15.25 


15.20 


14. 


73 


15.30 


15.25 


14.66 


15.27 


14.65 


12.0 


15.61 


14.75 


14.9 


15.33 


14. 


34 


14.99 




15.18 


15.27 


14.82 


12.3 


15.33 


14.72 


15.25 


15.29 


15. 


21 


15.18 


14.6 


15.69 


14.97 


15.15 


11.1 


15.46 


14.67 


15.25 


14.92 


13. 


93 


14.81 


15.4 


15.21 


15.32 


15.54 


10.5? 


15.37 


14.82 


15.45 


14.63 


14 


25 


15.05 


15.3 


15.02 


14.98 


15.36 


11.0 


15.60 


14.77 


15.5 


14.77 


15. 


32 


15.12 


15.4 


15.05 


15.07 


15.48 


11.0 


15.15 


14.68 


15.05 


14.25 


15. 


12 


15.03 


15.15 


15.46 


15.17 


15.55 


11.5 


15.69 


14.80 


14.55 


15.00 


14 


92 


14.78 


15.2 


15.18 


16.2 


15.68 


11.7 


15.11 


14.68 


15.25 


15.17 


14 


92 


14.95 


15.3 


15.33 


15.25 


15.40 


11.7 


15.35 


15.05 


14.95 


15.20 


15 


01 


15.32 


14.4 














14.95 










14.9 


15.18 


15.43 


15.03 


12.3 


15.31 


14.92 


14.6 


14.80 


14 


25 


14.96 


14.3 


15.16 


15.39 


15.73 




15.48 


14.57 


15.3 


14.89 


14 


13 


15.08 


14.3 


15.21 


15.33 


15.63 


11.5 


14.86 


14.66 


14.95 


14.89 


14 


10 


15.4 


14.85 


14.15 


14.80 


15.77 


11.7 


15.56 


14.53 


14.55 


14.37 


14 


06 


15.21 


15.25 


15.35 


14.92 


15.63 


11.7 


15.57 


14.65 


14.9 


14.8 


14 


34 


15.32 


15.05 


15.40 


15.22 


15.39 


12.5: 


15.27 


14.83 


15.0 


14.51 


14 


31 


14.98 


15.2 


14.70 


15.30 


15.02 


12.6 


15.60 


14.63 


15.2 


14.01 


13 


95 


14.87 




15.21 


14.83 


14.23 


12.5 


15.10 


14.65 




14.53 


14 


09 


15.13 


15.2 


15.07 


15.31 


14.82 


12.4 


15.52 


14.70 


14.55 


14.34 


14 


35 


14.91 




14.31 


14.82 


15.53 






14.50 




13.98 






15.06 


15.25 


15.59 


14.82 


15.42 


11.6 


15.56 


14.61 


14.65 


15.23 


15 


09 


15.14 




15.21 


15.12 


14.75 


12.0 


15.50 


14.80 


15.1 


14.63 


14. 


59 


15.10 


14,35 


15.08 


15.13 


14.91 




14.96 


14.90 


14.85 


15.33 


14 


79 


15.11 


14.9 


14.78 


15.27 


15.06 




15.31 


14.25 


14.7: 


13.60 


14 


00 


15.11 


15.25 


15.66 


14.94 


15.66 


12.2 


15.48 


14.52 


15.6 


15.0 


14 


32 


15.23 


15.45 


15.26 


14.95 


15.59 


12.1 


15.55 


14.65 




14.90 


14 


23 


15.20 


14.1 


15.12 


15.40 


15.62 


10.7 


15.34 


14.78 


14.55 


15.29 


14 


66 


15.11 


14.35 


15.50 


15.75 


15.41 


10.7 


14.75 


14.65 


15.2 


14.87 


14 


50 


15.41 


14.8 


15.41 


15.33 


15.56 


11.3 


15.49 


14.64 


14.9 


14.57 


14 


38 


15.02 


14.4 


14.26 


15.29 


15.6 


11.6 


15.49 


14.55 


15.25 


14.77 


14 


93 


15.07 


14.6 


15.48 


15.65 


15.65 


10.8 


15.16 


14.51 


14.95 


14.84 


14 


86 


15.1 



24 



Julian Day No. 28 No. 29 No. 30 No. 31 No. 32 No. 33 No. 34 No. 35 No. 36 

34540.613 
4572,602 
4573.635 
4574.602 
4575.603 
4929.623 
5273.612 
5274.609 
5275.610 
5307.600 
5308.599 
5309.600 
5310.600 
5658.601 
5661.602 
5685.588 
5687.592 
5688.590 
6752.607 
6753.602 
7113.610 
7115.636 
7116.640 
8198.614 
8199.629 
8584.628 
8586.605 
9262.779 

.785 
9265.585 

.680 

.684 

.772 

.816 

.819 

.847 
9270.772 

.776 

.798 

.803 
9271.615 

.619 

.647 

.651 

.697 

.701 

.722 

.725 

.771 

.776 

.817 

.820 



15.39 


15.58 


14.95 


15.48 


15.63 


15.2 


15.25 


14.86 


15.35 


15.25 


15.38 


14.75 


14.77 


15.50 


15.3 


15.25 


14.68 


15.05 


15.07 


15.41 


15.35 


15.08 


15.40 


15.5 


15.25 


15.16 


14.7 


15.12 


15.84 


15.74 


16.01 




15.5 


14.65 


15.52 


15.25 


14.78 


14.93 


14.91 


14.92 


14.57 


15.6 


15.45 


14.64 


15.15 


15.28 


15.39 


15.52 


15.35 


15.41 


15.6 


15.45 


14.95 




15.11 


15.22 


15.55 


14.87 


15.53 


15.5 


14.75 


14.81 


14.95 


14.60 


15.43 


15.33 


15.33 


14.36 


15.55 


14.95 


14.61 


15.25 


15.48 


15.93 


15.15 


15.41 


14.97 


15.5 


15.5 


14.65 


14.95 


15.40 


15.56 


15.13 


14.95 


14.57 


15.4 


14.8 


14.69 


14.95 


15.21 


15.70 


15.53 


15.35 


15.09 




15.6 


14.95 




15.37 


15.18 


15.60 


15.26 


15.49 


15.4 


15.25 


15.27 


15.15 


15.03 


15.01 


15.19 


14.90 


15.53 


15.25 
15.15 


14.95 
15.35 


14.69 


14.9 
15.15 






14.65 


15.16 


15.42 


15.1 


14.8 


15.04 


15.0 


15.34 


15.48 


15.55 


15.43 


15.54 


14.85 


15.2 


15.12 


15.2 


15.02 


15.48 


15.66 


15.17 


14.68 


14.85 


14.95 


14.53 


15.3 


14.62 


15.55 


15.46 


15.49 


15.27 


14.9 


15.3: 


14.76 




15.26 


15.74 


15.49 


15.47 


15.65 


15.7 


15.4 


15.07 


15.15 


14.80 


15.87 


15.01 


15.34 


15.30 


15.6 


14.95 


15.27 


15.2 


14.73 


15.05 


15.07 


15.38 


14.98 


15.4 


15.15 


14.65 


14.9 


15.36 


15.70 


15.28 


14.95 


15.47 


15.6 


15.25 


15.04 


15.15 


15.36 


15.55 


14.95 


15.38 


15.43 


15.6 


15.15 


14.72 


14.95? 


15.39 


15.57 


15.15 


14.90 


15.19 


15.3 


15.4 


14.87 


15.5 


15.12 


15.56 


15.15 


15.39 


15.45 


15.4 


15.4 


14.92 




15.24 


15,45 


14.84 


15.25 


15.50 




14.9 


14.94 


15.5 


14.59 


15.08 


15.34 


14.92 


15.44 


14.55 


15.7 


15.41 




15. 15: 


14.60 


15.20 


15.28 


15.41 






14.65 




15.29 


14.62 


15.21 


15.4 


15.48 


15.4 
14.55 


15.25 
15.5 


14.69 


14.9 


15.48 


15.48 


15.16 


14.96 


15.13 


14.9: 




14.83 




15.35: 


15.61: 


15.14 


15.28 


15.32 






14.97: 




15.40 


15.61 


15.38 


15.40 


15.55 


15.6 


14.5 


14.70 


14.85 


15.37 


15.63 


15.37 


15.35 


15.51 


15.3 


14.5 


14.64 


14.85 


15.55 


15.63 


15.51 


15.48 


15.67 


15.65 


14.65 


14.64 


14.7 


15.27 


15.67 


15.54 


14.87 


15.22 


15.4 


15.5 


14.62 


15.3 


15.35 


15.62 


15.49 


14.87 


15.28 


15.3 


15.4 


14.73 




15.07 


15.81 


15.49 


14.93 


15.31 


15.5 




14.41 


15.2 


15.31 


15.79 


15.58 


14.94 


15.29 


15.25 


15.5 


14.61 


14.9 


15.11 


15.58 


15.03 


14.83 


14.76 


14.55 


14.95 


15.03 


14.95 


15.45 


15.74 


15.06 


14.80 


14.90 


14.4 


14.95 


15.17 


15.0 


15.10 


15.61 


15.10 


14.73 


14.93 


14.6 


15.05 


14.80 


15.15 


15.31 


15.69 


15.09 


14.83 


15.10 


14.65 


14.95 


14.81 


15.15 


14.95 


15.85 


15.37 


14.78 


15.18 


15.05 


15.4 


14.30 


15.4 


15.40 


15.71 


15.17 


14.86 


15.31 


14.9 


15.05 


14.57 


15.0 


15.32 


15.36 


15.36 


15.01 


15.32 


15.25 


15.3 


14.52 


15.05 


15.43 


15.42 


15.27 


14.93 


15.43 


14.95 


15.3 


14.62 


15.15 


15.36 


15.03 


15.40 


15.27 


15.53 


15.5 
15.25 


15.25 
15.15 


14.67 


15.3 


15.38 


14.73 


15.45 


15.38 


15.58 


15.4 


15.25 


15.00 


15.3 


15.32 


14.77 


13.37 


15.30 


15.47 






14.93 





25 



No. 39 


No. 40 


No. 41 


No. 42 


No. 43 


No. 44 


No. 45 


No. 47 


No. 52 


No. 55 


15.33 


14.90 


15.64 




15.44 


14.56 


15.4 


14.73 


14.79 


15,13 


15.38 


15.42 


14.86 


11.7 


15.30 


14.90 


15.3 


15.20 


15.20 


15.23 


15.30 


14.84 


15.12 


11.6 


15.42 


15.02 




15.16 


15.21 


15.14 


14.76 


14.95 


15.00 


11.7 


15.24 


14.95 


14.7 


15.05 


15.09 




15.84 


15.01 


15.15 




15.51 


14.84 




14.75 


15.05 


15.30 


15.77 


14.89 


15.63 


11.3 


14.88 


14.90 


15.25 


15.25 


14.42 


14.78 


15.57 


15.03 


14.45 




14.96 


14.83 


14.95 


15.35 


14.62 


14.95 


15.35 


14.96 


14.31 


12.2 


15.40 


14.62 


14.65 


14.83 


14.48 


14.91 


14.98 


14.64 


14.25 


12.5 


14.67 


14.35 


15.15 


15.10 


13.92 


14.95 


15.37 


14.95 


15.55 


12,5 


15,49 


14.77 


15.1 


15.17 


14.31 


15.15 


14.98 


14.92 


15.65 


12.2 


15.00 


14.82 




14,84 


14.13 


15.19 


15.70 


15.17 


15.63 


12.4 


15,51 


15.00 


14.95 


14.95 


14.24 


15.28 


15.51 


15.23 


15.69 


11.9 
12.2 


14.85 


14.88 
14.98 


15.0 
15.25 


14.26 


14.25 


15.16 


15.15 


15.50 




12,9 


15.32 


14.81 


15.4 


14.90 


15.26 


15.31 


14.96 


14.83 


14.97 


12,1 


14.82 


14,67 


15.25 


14.98 


14.84 


15.39 


15.62 


15. 13 


15.16 




14.74 


14.60 


15.25 


14,95 


14.58 


15.37 


15.15 


15.27 


15.37 




15.39 


14.62 




14.73 


14.81 


15.30 


15.59 


15.20 


14.77 


11.4 


14.87 


14.67 


14.6 


15.60 


14.73 


15,13 


15.56 


15.06 


14.77 




15,57 


14.78 


15.15 


15.39 


14.18 


15.39 


15.48 


14.93 


14.33 


11,0 


15.25 


15.07 


15.0 


15.59 


15.13 


15.32 


14.45 


15.39 


15.06 


10.9 


14.98 


15.10 


15.25 


15.15 


15.15 


15.26 


15.53 


15.05 


15.18 


11.2 


15.51 


15.10 




15.05 


15.04 


15.25 


15.41 


15.19 


15.65 


10.8: 


15.22 


14.93 


14.6 


15.30 


14.29 


15.02 


15.03 


15.25 


15.62 




15.38 


14.94 




15.55 


14.14 


15.10 


15.56 


15.05 


15.45 


11.5 


15.10 


15.23 


14.7 


14.78 


15.16 


15.10 


15.1 


14.95 


14.92 


11.6 


15.21 


15.23 




15.51 


15.35 


14.94 


14.87 


14.87 


15.35 


12,1 


14.76 


14.70 




15.00 


14.55 


15.10: 


14.82 


14.92 


14.96 


12.4 


14.93 


14.65 


15,25 


15.16 


14.65 


15.1 


14.81 


14.70 


15.55 


12.2 
12.4 
12.2 


15.22 


14.58 




14.09 


14.82 


15.37 


14.93 


15.15? 


14.6: 


15.48 


14.77 




14.62? 


14.73 


14.96: 


15.22 


15.25 


14.79 


12.8 


15,42 


14.71 


15.5 


14.56 


14.28 


14.94 


15,27 


15.33 


14.90 


12,5 


15.46 


14.89 


15.1 


14.83 


14.37 


14.79 


15.41 


15.41 


14.95 


12.8 


15.61 


15.00 


15.2 


14.92 


14.09 


14.90 


15.54 


14.85 


15.20 


12.6 


15,17 


14.83 


15.4 


14.89 


14.74 


14,89 


15.50 


14.92 


15.35 


12,6 


15.21 


14.92 




15.10 


14.95 


14.90 


15.58 


14.83 


15,31 




15.24 


14.84 


15.3 


14.79 


14,40 


14.91 


15.60 


14.88 


15.41 


12.5 


15.22 


14.96 


14,9 


14.90 


14.73 


14.87 


14.77 


15.17 


14,51 


12,6 


15.42 


14.76 


14.5 


14.45 


14,96 


15.20 


14.63 


15.15 


14.27 


12.6 


15.48 


14.80 


14.7 


14.48 


15,08 


15.40 


14.95 


14.93 


14.73 


12,5 


15,49 


14.66 


14.85 


14.15 


14.87 


15.10 


14,91 


15.0 


14.65 


12,6 


15,55 


14.70 


14.75 


14,37 


15.14 


15.09 


15,36 


14.75 


14.85 




15,48 


14,67 


14.95 


14.21 


14.71 


14.92 


15,05 


14.81 


14.90 


12.8 


15,60 


14,63 


14,75 


14,49 


15.12 


14.83 


15.22 


14.93 


15.10 


12.8 


15,37 


14,46 


14,85 


14.41 


14,97 


14.90 


15.15 


14.85 


15.10 


12.8 


15.55 


14.78 


14,95 


14,74 


15.28 


14.81 


15.35 


15.05 


15.42 


12,6 
12.5 


15.55 


14.90 


15,15 

14.85 


14.78 


14,91 


14.91 


15.44 


15.15 


15.30 


12.5 


15.47 


15.02 


15.25 


14.90 


14,58 


15.13 


15.42 


15.22 


15.50 


12.4 


15.53 


14.97 




15.12 


14,55 


15.02 



26 



Julian Day No. 58 No. 59 No. 61 No. 62 No. 63 No. 64 No. 65 No. 66 No. 67 

28308.736 15.25 15.05 

8309.651 

.661 14.65 14.93 15.51 15.60 15.35 15.1 15.15 15.40 

.670 14.76 15.02 15.42 15.36 15.45 14.85 15.15 15.36 

.677 14,86 15.01 15.38 15.36 15.5 14.85 15.10 

.796 15.41 15.32 15.51 14.97 15.45 15.05 14.86 15.17 

8365.608 15.46 15.27 14.62 15.51 14.95 15.6 14.41 15.05 

8366.608 15.16 15.13 15.47: 14.98 14.8 15.5 14.57 15.10 
8399.596 15.02 14.94 15.46 15.30 14.95 14.9 15.25 14.90 
8688.640 14.65 14.7 

8692.632 15.55 15.30 14.96 15.30 14.65 15.05 15.05 15.45 15.25 

8693.730 15.44 15.37 14.91 15.35 14.95 15.05 15.2 15.48 

8696.631 15.60 14.90 15.03 15.32 14.65 15.6 15.22 15.20 15.05 

9071.660 15.09 14.62 15.42 15.29 15.45 15.15 14.68 15.29 

9072.698 15.23 14.60 15.40 15.17 15.2 15.25 14.65 15.11 15.7 

9073.605 15.18 15.42 15.00 15.36 15.25 15.0 14.53 15.5 15.15 

9076.603 15.25 

9078.600 15.1 15.0 14.85 

9079.602 15.30 15.20 15.34 15.20 15.35 14.85 14.92 15.35 14.9 

9786.609 15.65 14.78 14.69 14.98 15.25 15.7 14.92 15.42 14.5 
9787.608 15.60 14.64 15.60 15.51 15.25 15.35 14.95 15.50 14.6 

9813.610 15.56 15.01 15.48 14.97 15.25 15.65 15.16 15.36 

9814.612 15.53 15.33 15.23 15.43 15.35 15.75 15.31 15.62 15.15 

9815.613 15.51 15.37 14.68 14.90 15.25 15.7 15.30 15.47 

9816.611 15.32 15.40 15.42 15.41 15.35 15.5 15.18 15.25 
30171.617 15.15 15.30 15.0 15.00 15.25 15.5 15.01 15.5 14.95 

0172.615 15.14 15.11 15.55 15.44 15.25 15.4 15.08 15.4 15.05 

0519.606 15.64 15.24 15.02 15.18 14.5 15.55 15.04 15.44 14.75 
0520.606 15.50 15.24 15.71 15.04 14.5 15.7 15.11 15.52 15.15 
0550.608 15.28 15.20 15.37 15.08 15.25 14.55 14.95 14.94 15.05 

0553.604 15.51 14.81 15.44 15.13 15.35 14.65 14.00 15.75 

0554.614 14.47 15.77 14.83 15.45 15.75 13.96 15.57 
0555.629 15.21 15.20 15.40 15.55 15.35 15.7 14.75 15.23 
0556.620 15.33 15.06 15.03 15.35 15.65 14,68 15.01 
0586.572 15.58 14.38 15.56 15.31 15.35 15.65 15.07 15.33 15.05 
0880,592 15.25 15.55 14.9 

.623 15.70 15.38 14.59 15.40 15.25 15.55 14.98 14.90 14.9 

,659 15,45 15,30 14.70 15.38 15.35 15.55 14.96 15.02 14.95 

,690 15,70 15.35 14.88 15.45 15.45 15.55 15.2 15.10 15.2 

.730 15.57 15.34 14.89 15.07 15.35 15.55 15.10 15.28 15.15 

.760 15.65? 15.37 15.08 14.99 15.35 15.7 15.22 15.44 15.6 
.788 

30883.630 15.59 14.42 15.21 15.01 15.25 15.0 15.15 15.45 15.45 

.664 15.69 14.75 15.35 15.23 15.35 15.1 15.31 15.53 15.6 

0884.622 14.7 15.15 

.651 14.6 15.4 

.680 15.66 14.45 14.95 14,92 15.35 14.75 15.26 15.46 15.75 

.721 15.65 14.64 15.23 15.05 15.45 15.05 15.27 15.50 15.35 

,771 15,5 14.90 15.30 15.10 15.35 15.15 14.03 15.11 15.1 



No. 68 No. 69 No. 70 No. 71 No, 72 No. 73 No. 74 No. 75 No. 76 No. 77 No. 78 



27 







15.15 
































14.95 
































15.0 


14.63 


15. 


7 






15.30 


14.26 


15.17 


15. 


10 


14. 


84 


15.20 






15.05 


14.78 


15. 


51 


15. 


48 


15.31 


14.30 


15.07 


14. 


99 


14, 


84 


15.22 








14.79 










15.33 


14.34 


14.95 


15. 


20 


14. 


96 


15.20 






15.55 


15.45 


15. 


45 


14. 


51 


15.17 


14.35 


15.05 


14, 


66 


14, 


82 


14.95 






15.15 


15.24 


14. 


85 


15. 


53 


14.98 


14.42 


15.40 


14, 


97 


14, 


94 


15.00 






15.35 


15.12 


14. 


53 


15. 


01 


15.01 


14.35 


15.10 


15, 


24 


15. 


01 


15.26 








14.64 










14.87 


14.40 


15.30 


15, 


12 


15, 


23 


15.20 






14.7 




























15 


25 


14.9 


15.62 


15. 


61 


15. 


5 


15.47 


14.14 


15.35 


15, 


16 


14, 


80 


15.14 


14 


9 


15.15 


15.59 


14. 


84 


15. 


5 


15.42 


14.33 


15.28 


14. 


83 


15, 


18 


15.0 


15 


45 


15.15 


15.8 


15. 


80 


15. 


85 


15.08 


14.45 


15.45 


15, 


00 


15. 


29 


15.02 


15 


65 


15.25 


15.47 


15. 


38 


15. 


16 


15. 17 


14.36 


15.32 


14, 


84 


15, 


20 


15.01 


15 


3 


15.0 


15.18 


15. 


48 


15. 


67 


15.02 


14.06 


15.25 


15. 


22 


15. 


30 


15.06 


15. 


4 


15.8 
14.7 




15. 


15 


15. 


52 


15.63 


13.96 


15.35 


15. 


21 


15. 


16 


15.29 


15 


25 


14.65 


15.47 


14. 


77 


15. 


15 


15.28 


14.42 


15.25 


15. 


01 


14. 


66 


15.06 


15 


4 


15.9 


15.60 


15. 


13 


15. 


59 


14.90 


14.45 


15.42 


15. 


11 


15. 


20 


15.04 


15 


7 


15.7 


14.92 


14. 


85 


15. 


51 


14.85 


14.28 


15.35 


15. 


17 


15. 


39 


15.40 


15. 


05 


15.75 


15.68 


15. 


75 


15. 


63 


15.39 


13.84 


15.37 


14, 


98 


15. 


15 


15.06 


15 


3 


15.6 


15.74 


15. 


87 


15. 


56 


15.37 


14,38 


15.65 


14. 


95 


15 


37 


15.33 








15.15 






14. 


63 


15.03 


14.35 


15.10 


15. 


23 


14. 


92 


15.28 








14.85 


15. 


34 


15. 


07 


15.11 


14.41 


15.25 


14 


95 


14. 


82 


15.11 


15 


2 


15.75 


15.8 


15. 


44 


15. 


22 


14.85 


14,46 


15.42 


15 


03 


14. 


91 


15.22 


15 


05 


15.75 


15.65 


15. 


49 


15. 


11 


14.95 


14,37 


14.95 


14 


81 


15. 


10 


15.30 


14 


65 


15.3 


15.39 


15. 


25 


14. 


49 


14.87 


13.94 


15.02 


14 


97 


14. 


9 


15.15 


15 


15 


15.4 


15.63 


15. 


61 


15. 


55 


14.90 


14.30 


15.46 


15 


02 


14 


78 


15.28 


15 


05 


15.35 


14.78 


15. 


38 


15 


00 


14,90 


14.50 


15.31 


14 


76 


15. 


11 


15.04 


15 


15 


15.5 




15. 


70 


15. 


35 


14.65 


14.0 


15.24 


14 


57 


14 


74 


15.11 








15.29 










14.77 


14,03 


15.33 


15 


27 


15. 


15 


14.77 








14.90 










14,80 


14,30 


15.69 


14 


93 


15. 


22 


14.95 








15.60 










14.78 


14,78 


15.24 


14 


74 


15 


33 


15.26 


15 


05 


15.25 
15.3? 


15.47 


14 


84 


15 


08 


14.75 


14.22 


14.96 


14 


97 


14 


75 


15.26 


15 


55 


15.55 


14.90 


15. 


44 


15 


23 


15.49 


14.30 


14.87 


15 


05 


14 


63 


14.92 


15 


.5 


15. 55 


14.86 


15 


51 


15 


35 


15,26 


14.27 


15.06 


15 


22 


14 


83 


14.94 


15 


5 


15.55 


15.0 


15 


58 


15 


49 


14.98 


14.27 


15.19 


15 


35 


14 


99 


15.11 


15 


.25 


15.6 


15.2 


15 


60 


15 


42 


14.95 


14.34 


15.23 


15 


29 


14 


95 


15.21 


15 


.2 


15.65 


15.45 


15 


60 


15 


58 


15.03 


14.37 


15.29 


15 


28 


15 


03 


15.33 


15 


.35 


15.65 


15.46 


15 


34 


15 


42 


15.44 


13.55 


15.30 


15 


00 


15 


28 


15.24 


15 


.5 


15.70 
15.5? 
15.35 


15.69 


15 


58 


15 


52 


15.59 


13.80 


15.39 


15 


18 


15 


40 


15.4 


15 


.6 


15.7 


14.50 


15 


65 


15 


55 


15.49 


14.20 


15.30 


15 


12 


15 


02 


15.26 


15 


.4 


15.4 


15.61 






15 


66 


15.45 


14.38 


15.22 


15 


08 


15 


00 


15.40 



15.05 15.5 15.36 15.43 15.39 15.05 14.28 15.06 14.92 14.77 15.17 



28 



Julian Day 


No. 58 


No. 59 


No. 61 


No. 62 


No. 63 


No. 64 


No. 65 


No. 66 


No. 6'i 


30899.602 


14.78 


15.37 


15.33 


14.92 


15.35 


15.65 


15.05 


15.22 


15.25 


.647 


15.42 


15.34 


15.52 


14.90 


15.45 


15.5 


14.04 


15.07 




.701 


15.56 


15.38 


15.60 


15.24 


15.5 


15. 55 


14.3 


15.40 




0900.604 


14.95 


15.16 


14.75 


15.31 


15.25 


15.35 


14.1 


14.87 


14.95 


.638 


15.46 


15.35 


15.12 


15.42 


15.5 


15.55 


14.35 


15.18 




0901.676 


15.69 


15.21 


14.77 


15.36 


15.55 


15.3 


14.93 


14.99 




0932.604 




15.15 


15.42 


15.12 


15.55 


14.9 


14.75 


15.10 




0933.589 




14.85 


14.90 




15.5 


15.5 








1257.634 


15.36 


14.39 


14.46 


14.95 


14.4 


14.35 


15.07 


15.55 


14.7 


1258.625 










14.5 


15.4 






14.9 


1259.604 


15.56 


15.25 


15.53 


14.99 


14.6 


15.5 


15.25 


15.33 


15.3 


1969.736 


15.56 


15.16 


15.33 


15.45 


15.65 


15.8 


14.64 


15.30 


15.25 


1976.641 


15.56 


15.32 


15.45 


14.94 


15.5 


15.5 


15.21 


15.08 


15.4 


1977.690 


15.71 


15.33 


15.31 


14.91 


15.5 


15.5 


15.15 


15.12 


15.45 


2000.641 


15.41 


15.40 


15.46 


15.30 


14.85 


15.65 


15.18 


15.25 


15.05 


2004.652 


15.95: 


15.00 


15.54 


15.43 


14.5 


14.9 


15.10 


15.65 


15.2 


2006.599 


15.29 


15.63 


14.73 


15.23 




15.3 


14.78 


14.85 


14.7? 


2326.715 


14.60 


15.20 


14.86 


15.05 


14.5 


15.5 


15.18 


14.82 




2328.739 


14.78 


14.63 


15.38 


15.25 


14.95 


15.05 


14.00 


15.11 




2354.604 


15.60 


15.53 


15.10 


15.12 


14.95 


15.6 


14.38 


15.38 


14.95 


2355.607 


15.09 


15.32 


14.97 


15.47 


15.15 


15.4 


13.78 


14.98 


14.9 


2356.605 


15.59 


15.37 


15.57 


15.07 


15.0 


15.3 


14.36 


15.03 


14.9 


2357.604 


14.78 


15.21 


15.35 


14.91 


15.25 


14.95 


14.36 


14.93 


14.9 


2361.704 


15.35 


14.48 


15.49 


15.34 


15.4 


15.6 


15.20 


15.08 


15.25 


2733.605 










15.5 


15.4 








2734.604 


15.90 


14.85 


15.48 


15.35 


15.3 


15.5 


15.05 


15.27 


15.15 


2740.608 


15.79 


14.31 


14.48 


14.75 


15.4 


15.35 


14.42 


15.48 


15.0 


2741.607 


15.75 


15.70 


15.74 


15.51 


15.4 


15.6 


14.85 


15.06 


15.0 


2742.648 


16.0 


15.32 


15.60 


14.87 


15.4 


15.4 


14.23 


14.93 


14.85 


2770.576 


15.64 


15.12 


15.45 


15.28 


14.25 


15.3 


14.69 


15.34 


15.05 


3068.668 


15.55 


14.98 


14.97 


15.46 


14.5 


14.65 


14.95 


15.2 


15.25 


3069.654 


15.65 


14.40 


15.49 


14.97 


14.65 


15.6 


14.71 


15.4 




3095.604 


14.85 


14.45 


15.27 


15.58 


14.5 


15.6 


15.18 


15.33 


14.9 


3096.609 


15.12 


15.36 


14.74 


14.81 


14.5 


15.25 


15.08 


15.69 


15.2 


3476.602 


15.56 






15.21 


15.2 


15.05 


14.09 


14.81 


14.9 


3477.601 


15.51 


15.30 


14.80 


15.35 


15.5 


14.75 


14.43 


14.92 


15.05 


3481,597 


14.95 


14.62 


14.93 


14.81 


15.5 


15.5 


15.10 


15.20 


14.95 


3505.572 


15.88 


15.25 


15.39 


14.93 


15.5 


15.4 


15.08 


15.36 


15.15 


3823.649 


15.36 


14.46 


15.39 


15.39 


15.0 


15.4 


14.10 


15.65 


15.3 


3858.636 


15.53 


15. 32 


15.05 


15.32 


15.25 


15.55 


15.13 


15.08 


15.5 


3860.589 


15.56 


15.21 


15.44 


15.27 


14.9 


15.4 


14.96 


15.31 


14.95 


4180.634 


15.28 


15.45 


15.48 


14.87 


14.95 


14.95 


15.35 


15.39 


15.05 


4181.607 


15.24 


15.34 


14.84 


15.55 


14.8 


14.75 


15.11 


14.00? 


14.95 


4182.607 


15.20 


15.14 


14.78 


14.91 


14.95 


15.6 


14.98 


14.84 


15.6 


4538.633 


15.75 


14.95 


14.69 


15.07 


15.45 


15.6 


14.92 


15.00 


15.4 


4539.634 


15.80 


14.53 


15.62 


15.35 


15. 5 


15.55 


14.88 


14.96 


15.55 


4540.613 


15.82 


15.05 


15.5 


15.19 


15. 5 


15.25 


14.85 


15.15 


14.95 


4572.602 


15.77 


15.10 


15.67 


14.90 


15.5 


14.75 


14.61 


14.83 


15.05 


4573.635 


15.70 


15.32 


15.46 


15.26 


15.45 


14.65 


15.01 


14.88 


15.1 



68 No. 69 No. 70 No. 71 No. 72 No. 73 No. 74 No. 75 No. 76 No. 77 No. 78 



29 



15.0 



15.8 15.45 15.17 15.21 15.65 14.16 15.32 14.82 15.20 15.34 



15.25 15.7 14.82 15.20 15.05 15.47 14.18 15.57 15.10 15.30 14. 



15.6 


15.7 


15.18 


15.63 


15.4 


15.31 


14.15 


15.67 


15.29 


15.29 


14.96 


15. 15 


15.6 


15.92 


15.39 


15.77 


15.60 


14.40 


15.05 


15.27 


15.31 


15.41 












15.58 


14.35 


15.30 


15.25 


15.35 


15.26 












15.44 


14.42 


15.63 


14.86 


14.72 


15.18 






14.82 






15.58 


14.14 
13.85 


15.72 


15.36 


15.37 


15.16 


15. 15 




15.21 


15.82 


15.61 


15.25 


14.13 


14.90 


14.88 


14.83 


15.20 


15.15 


15.5 


15.75 


15.58 


14.91 


15.08 


13.92 


15.20 


14.95 


15.25 


15.04 


15.25 


15.25 


15.80 


15. 85 


15.39 


15.26 


14.41 


15.23 


14.95 


15.39 


15.06 


15.05 


14.95 


15.31 


15.60 


15.51 


14.92 


14.23 


14.89 


14.74 


14.71 


14.96 


15.15 


15.5 


14.90 


15.85 


15.60 


14.91 


14.33 


15.58 


15.10 


14.81 


15.12 


14.9 


15.65 


15.41 


15.42 


15.25 


15.39 


14.32 


15.05 


15.20 


15.18 


15.26 


14.85 


15.7 


15.98: 


15.66 


15.49 


15.63 


14.05 


15.18 


15.03 


14.70 


15.37 


14.85? 




15.51 


15.18 


15.60 


14.95 


14.44 


15.18 


14.58 


14.80 


14.80 


15.1 


15.6 


14.48 


15.32 


14.60 


15.12 


14.12 


15.50 


15.32 


14.89 


15.00 


15.35 


15.6 


15.70 


15.45 


15.70 


15.22 


13.92 


15.57 


14.79 


15.18 


15.18 


15.05 


15.6 


14.99 


15.51 


15.48 


14.90 


13.83 


15.82 


14.85 


14.91 


14.87 


14.9 


15.5 


15.40 


15.02 


14.91 


14.85 


13.97 


15.36 


15.18 


15.25 


14.83 


14.9 


15.4 


15.33 


14.98 


14.56 


14.83 


14.35 


15.16 


14.94 


15.28 


15.19 


15.05 


15.35 


15.04 


15.14 


14.43 


14.90 


14.36 


15.10 


14.80 


15.35 


15.36 


14.85 


15.25 


15.59 


15.31 


15.30 


15.05 


14.29 


15.56 


15. 18 


15.38 


14.88 


15.2 


15.55 




















14.9 


15.3? 


14.86 


14.42 


15.21 


15.33 


13.90 


15.33 


14.94 


15.26 


14.90 


14.95 


15.6 


14.78 


14.24 


14.66 


15.05 


14.25 






14.74 


15.32 


15.05 


15.6 


15.83 


14.16 


15.26 


14.82 


14.13 


15.07 


14.89 


14.85 


15.36 


14.9 


14.6 


15.85 


14.48 


15.65 


14.98 


14.13 


15.44 


14.98 


15.02 


15.25 


15.25 


15.5 


15.85 


15.83 


15.55 


15.36 


14.16 


15.20 


14.85 


15.08 


15.00 


15.05 


15.55 


15.52 


15.13 


15.65 


15.22 


14.05 


15.30 


15.20 


14.80 


15.20 


15.05 


15.7 


14.83 


15.92 


15.48 


15.25 


13.93 


15.54 


15.13 


14.92 


15.04 


15.05 


15.0 


15.39 


15.64 


15.69 


14.75 


13.89 






15.02 


14.87 


15.2 


15.25 


16.02 


15.90 


15.43 


14.95 


14.40 


14.73 


14.64 


14.76 


15.00 


15.2 


14.75 


15.19 


15.41 


15.37 


14.77 


14.25 


15.55 


15.10 


15.43 


14.72 


15.4 


14.9 


15.43 


15.69 


14.81 


14.42 


14. 16 


15.42 


14.80 


14.71 


15.10 


15.15 


14.9 


15.78 


15.59 


14.88 


15.17 


14.30 


15.30 


14.90 


15.29 


14.94 


14.95 


15.4? 


15.53 


15.67 


15.73 


15.29 


14.28 


15.29 


14.93 


14.73 


15.31 


14.85 


15.5 


15.0 


15.8 


15.32 


15.35 


14.20 


15.59 


15.05 


15.17 


15. 12 


15.3 


14.9 


15.61 


14.5 


15.41 


15.3 


13.52 


15.62 


15.18 


15.45 


15.26 


15.0 


14.55 


15.10 


14.79 


14.68 


14.94 


14.24 


15.30 


14.79 


14.84 


15.01 


14.95 




15.02 


15.52 


15.20 


14.98 


14.19 


15.44 


14.76 


15.39 


15.37 


15.25 


15.4 


14.30 


15.42 


15.04 




14.20 


14.95 


15.15 


14.66 


15.01 


15.3 


15.65 


15.12 


15.68 


15.59 


14.58 


14.43 


15.36 


15.11 


14.71 


15.00 


15.25 


14.9 


14.91 


15.53 


14.81 


14.90 


14.27 


15.31 


14.85 


15.15 


15.36 


15.05 


15.05 


15.35 


15.58 


15.69 


15.25 


13.79 


15.37 


14.86 


15.25 


15.40 


15.25 


14.85 


16.10 


15.62 


15.75 


15.25 


14.01 


15.65 


15.29 


15.39 


14.85 


15.25 


15.6 


14.60 


14.00 


15.33 


15.15 


14.20 


15.45 


15.20 


15.38 


15.26 


15.15 


15.5 


15.56 


14.73 


15.32 


15.20 


14.30 


15.06 


14.89 


15.19 


15.18 



30 



Julian Day 


No. 58 


No. 59 


No. 61 


No. 62 


No. 63 


No. 64 


No. 65 


No. 66 


No. 6^ 


34574.602 


15.85 


15.55 


15.60 


14.85 


15.4 


15.7 


15.03 


14.92 


15.45 


4575.603 


15.76 


15.26 


14.69 


15.45 


15.55 


15. 55 


15.00 


15.23 


15.25 


4929.623 


16.0 


15.39 


15.70 


15.49 


14.9 


15.45 


14.59 


15.09 


15.4 


5273.612 


15.95 


15.07 


15.61 


14.84 


15.2 


15.45 


15.31 


14.87 


14.85 


5274.609 


15.68 


14.53 


15.28 


15.40 


15.1 


15.45 


14.94 


15.13 


14.9 


5275.610 


15.93 


14.85 


14.81 


15.13 


15.25 


14.9 


14.99 


15.06 


15.3 


5307.600 


15.08 


14.85 


15.45 


15.28 


15.45 


14.7 


14.99 


15.07 


14.95 


5308.699 


15.21 


15.47 


14.91 


15.18 


15.35 


15. 55 


15.10 


15.08 


14.9 


5309.600 


15.13 


15.55 


15.60 


14.96 


15.3 


15.45 


15.27 


15.45 


14.9 


5310.600 


14.98 


15.29 


15.59 


15.30 


15.15 


15.5 


15.13 


15.42 


14.85 


5658.601 




15.45 








15.45 






14.9 


5661.602 


14.94 


14.37 


14.66 


15.12 


14.3 


14.95 


15.09 


15.15 




5685.588 


15.57 


15.18 


14.92 


14.89 


14.8 


14.85 


15.19 


15.21 


14.95 


5687.592 


15.77 


14.30 


15.70 


14.91 


14.7 


15.7 


14.89 


15.25 


15.3 


5688.590 


15.57 


15.34 


15.28 


15.41 


14.9 


15.7 


13.84 


15.49 




6752.607 


15.51 


15.27 


15.43 


15.53 


14.9 


15.6 


14.88 


15.10 


15.55 


6753.602 


15.82 


15.43 


15.37 


15.15 


14.7 


15.55 


15.03 


14.70 




7113.610 


15.43 


15.16 


15.62 


15.46 


15.4 


15.6 


15.12 


15.40 


15.4 


7115.636 


15.8 


15.41 


14.63 


15.8: 


15.15 


15.6 


15.12 


15.50 


15.6 


7116.640 


15.84 


15.30 


15.16 


15.09 


15.4 


15.3 


14.13 


15.23 


15.25 


8198.614 


15.27 


15.33 


15.49 


14.90 


15.5 


15.4 


15-00 


15,66 


15.3 


8199.629 


15.00 


15.30 


15.24 


15.36 


15.5 


15.25 


14.52 


15.28 


15.25 


8584.628 


15.51 


15.43 


15.73: 


15.37 


15.05 


15.6 


15.37 


14.95 


15.25 


8586.605 


15.76 


15.31 


15.40 


15.35 


15.05 


14.85 


14.56 


15.25 


14.85 


9262.772 










14.85 










.779 


14.63 


14.45 


14.55 


15.38 


14.7 


15.55 


15.01 


15.38 


14.85 


.785 


14.89 


14.36 


14.61 


15.37 


14.7 


15.5 


15.06 


15.30 


14.9 


9265.585 










15.35 


14.8 






14.8 


.620 












14.85 






14.85 


.680 


14.75 


14.97 


15.23 


15.34 




15.35 


14.97 


14.97 


15.15 


.772 


15.2 


15.26? 


15.31 


14.92 




15.6 


15.29: 


15.29: 


15.3? 


.816 


15.31 


15.28 


15.30 


15.22 


14.45 


15.4 


14.06 


15.34 


15.2 


9265.819 


15.46 


15.38 


15.51 


15.07 


14.55 


15. 55 


14.20 


15.37 




.847 


15.35 


15.41 


15.57 


15.37 


14.55 


15.6 


14. 13 


15.57 


14.85 


9270.772 


15.62 


15.35 


14.72 


14.92 


14.6 


15.6 


14.84 


15.37 


14.9 


.776 


15.62 


15.33 


14.83 


14.86 


14.65 


15.55 


15.02 


15.40 


14.8 


.798 


15.80 


15.30 


15.08 


14.93 


14.45 


15.55 


14.86 


15.50 


14.9 


.803 


15.80 


15.41 


14.92 


14.77 


14.4 


15.6 


14.95 


15.55 


14,9 


9271.615 


14.74 


15.06 


15. 55 


14.72 


15.5 


14.85 


14.21 


15.05 




.619 


14.78 


15.19 


15.72 


14.86 


15.4 


14.85 


14.44 


14.94 


15,15 


.647 


14.94 


15.09 


15.38 


14.77 


15.5 


15.05 


14.25 


14.97 


15.4 


.651 


14.99 


15.11 


15.62 


14.84 


15.5 


14.9 


14.54 


14.95 


15.9 


.697 


15.38 


15.46 


15.69 


14.95 


15.55 


15.1 


14.66 


14.84 


15.4 


.701 


15.32 


15.28 


15.72 


14.94 


15.4 


14.95 


14.74 


15.07 


15.6 


.722 


15.33 


15.21 


15.47 


15.05 


15.6 


15.25 


14.61 


15.12 


15.3? 


.725 


15.50 


15.35 


15.68 


15,02 


15.4 


15.15 


14.91 


15.15 




.761 


15.70 


15.33 


15.67 


15.33 


14.55 


15.4 


14.95 


15.45 


14.9 


.776 










14.25 


15.5 






15,15 


.817 


15.56 


15.28 


15.27 


15.45 


14.45 


15.6 


15,07 


15.32 




.820 


15.53 


15.32 


15.18 


15.35 


14.6 


15.5 


14.97 


15.58 


14.85 



31 



No. 68 No. 69 No. 70 No. 71 No. 72 No. 73 No. 74 No. 75 No. 76 No. 77 No. 78 



15.15 

15.15 

15.25 

15.4 

15.45 

15.15 

15.05 

14.85 

14.85 

14.9 

15.25? 

14.95 

14.4 

14.55 

14.5 

14.8 

14.7 

15.05 

14.8 

14.85 

14.75 

14.7 

14.9 

15.05 



15.7 

15. 55 

15.05 

15.4 

15. 35 

15.4 

14.8 

14.6 

14.7 

15.05 

15.25 

15.2 



15. 
15. 
14. 



14.15 

14.4 

15.6 

15.6 

15.4 

14.8 

14.4 

14.85 

14.8 



15.21 
15.23 
15.06 
14.75 
15.77 
15.13 
15.69 
15.52 
15.54 
15.16 

15.35 

15.63 

14.73 

15.21 

15.73 

15.19 

15.21 

15.73 

15.46 

15.75 

15.7 

15.54 

15.60 



14.51 
14.72 
15.90 
14.95 
14.93 
14.69 
15.66 
15.47 
15.55 
15.51 

15.34 

14.27 
14,16 
14.51 

15.10 
14.25 
14.35 
14.36 

15.48 

15.28 
15.44 
15.38 



14.45 

15.47 

15.4 

15.05 

15.74 

15.57 

15.57 

15.15 

14.77 

15.34 

14.91 
15.53 
15.30 
15. 16 
14.57 
14.62 
15.55 
15.12 
14.87 
15.25 
14.74 
15.45 
15.03 



15.15 

15.25 

15.23 

15.43 

15.50 

15.25 

15.51 

15.49 

15.59 

15.40 

15.25 

15.23 

14.87 

14.69 

14.85 

14.85 

14.95 

15.28 

15.56 

15.28 

16.0 

15.56 

15.28 

15.43 



13.42 
14. 19 
13.50 
14.29 
14.20 
13.79 
14.39 
14.34 
13.57 
13.96 
14,28 
14.57 
13.88 
14.05 
14,32 
14,02 
13,88 
14,15 
13.85 
14.10 
14.34 
14.28 
14,36 
14,08 



15,63 
15,64 
15,35 
15.06 
15,30 
15.20 
15.39 
15.28 
15,49 
15.15 

14,85 
15,49 
15.17 
15,48 
15,07 
15,64 
15.48 
15.39 
14.99 
15.47 
15.16 
15.42 
15.40 



15.01 
15. 19 
14.73 
15.20 
14.83 
14.89 
14.79 
15,15 
15,09 
14.71 

14,79 
15,30 
14,86 
14,81 
15,17 
14.85 
15.28 
14.89 



16 

99 



14.79 
14.95 
15.20 



14.91 
14,95 
14,75 
14,79 
14,91 
15.28 
15.02 
15.34 
15.43 
15.01 

14,82 
15.38 
14.78 
14,84 
14.88 
15.30 
15.10 
15.34 
15.07 
14.78 
15.07 
15,03 
15, 12 



15.07 
14,79 
14.66 
14.97 
15.33 
15.01 
15.07 
14.86 
15.25 
15.34 

15.13 
15.23 
14.75 
14.86 
14.87 
14.97 
14.82 
15.29 
15.21 
14.96 
14.75 
15.03 
15. 12 



15.25 

15.2 

14.9 

14.85 

15.25 



15. 
15, 



15 

2 



15.25 
15.35 



15. 
15, 



15,3 

14,95 

14,9 

15,15 

15.15 

15.4 

15.1 

15.25 

15.2 

15.35 

15,3 

15.2 

15.15 



15.4 
14.5 
14.5 

14.85 



15. 
15. 



15.6 
15.7 
15.65 
15.7 



14.95 

15.25 

15.25 

15.6 

15.6? 

15.6 

15.6 

15.65 

15.65 

15.7 
15.5 



15.28 
15.36 



15.00 

15.31 

15,43 

15.65 

15.46 

15,27 

15,35 

15,4 

15,35 

15,58 

15.92 

15,58 

15,76 

15,50 

15,91 

15.05 

15.20 

14.73 

14.90 
14.93 



14.63 
15,0 



15,05 

14,97 

15.07 

15,16 

15,26 

14,5 

14,67 

14.79 

14,89 

15.25 

15.53 

15.27 

15.41 

15.37 

15.61 

14.70 

14.60 

14.56 

14.92 
14.92 



15.03 15,74 14.42 15.35 15.06 15,13 15.31 
15,13 15,63 14,32 15,30 15,05 15,05 15,34 



14.55 
15.12 
15.26 
15.20 

14.73 
14.83 
14.91 
14.89 
15.09 
15.42 
15.07 
15.31 
15.53 
15.78 
15.58 
15.67 
15.42 



14.85 

15.27: 

15.34 

15.46 

15,51 

14,89 

15.06 

15,05 

14,73 

15,41 

15,60 

15,55 

15,51 

15,36 

15,48 

15.11 

14.95 



13.78 
14.23 
14.08 
14.15 
14.03 
14.00 
13,93 
14,03 
14.15 
13,84 
13,77 
13,97 
14,02 
13,72 
14.07 
14,07 
14,11 
14,25 



15,60 

15.35: 

15,57 

15.47 

15,56 

15,23 

15. 10 

15,19 

15,01 

14,85 

15.09 

15.21 

15,20 

15.28 

15.15 

15.27 

15.16 

15.34 



15.00 

14.76: 

15.14 

14.93 

15.25 

15,11 

15,04 

14.96 

14,85 

15.01 

15.06 

14.83 

14.90 

14.87 

14.80 

14.90 

14.68 

14.77 



15.46 
15.23 
14,90 
14.77 
14.90 
15,51 
15.36 
15, 55 
15,46 
15,39 
15.51 
15,40 
15,38 
15.32 
15.05 
14.90 
14.79 
14.79 



15,07 

14.92: 

14.81 

14.90 

15.06 

14,95 

15. 10 

14.71 

14.79 



14,80 
14.94 
14.90 
14.83 
15.15 
15.23 
15.27 
15.34 



14.89 14.87 
14.79 14,73 



14,27 15.55 14.90 14.73 15.06 
14.30 15.42 14.87 14.64 15.06 



32 



Julian Day 


No. 79 


No. 80 


No. 81 


No. 83 


No. 84 


No. 87 


No. 92 


No. 98 


28309.651 










12.2 








.661 


15.05 


14.97 


15.55 


15.5? 


12.2 


14.85 


14.44 




.670 


15.05 


14.97 


15.39 




12.2 


14.84 


14.44 




.677 


14.97 


14.90 


15.30 




12.1 


14.92 


14.46 




.796 


14.78 


14.70 


14.67 


14.75 


11.9 


15.02 


14.27 


15.15? 


8365.608 


15.17 


14.85 


15.07 


15.05 


11.9 


14.98 


14.23 


15.1 


8366.608 


15.10 


14.84 


14.58 


15.7 


11.0 


15.03 


14.37 


15.5 


8399.596 


15.15 


15.07 


15.02 




11.2 


15.12 


14.58 


15,0 


8688.640 










10.7 








8692.632 


14.86 


15.18 


14.57 


14.4 


11.2 


15.16 


13.93 


15,4 


8693.730 


15.14 


15.03 


14.92 


14.95 


11.4 


15.12 


14.36 


15.05 


8696.631 


14.85 


15.29 


14.97 


15.0 


11.6 


15.12 


14.38 


15.6 


8715.638 










11.3 








9071.660 


14.79 


14.92 


14.73 


14.6 


11.4 


14.99 


13.92 


15.7 


9072.698 


14.92 


14.96 


15.02 


15.6 


12.1 


15.25 


14.40 


15.05 


9073.605 


15.20 


15.23 


15.40 


15.55 


11.7 


15.20 


14.25 


15.05 


9077.600 








15.25 










9079.602 


15.04 


15.15 


15.07 


15.3 


10.8 


15.04 


14.07 




9786.609 


14.84 


15.00 


14.93 


15.0 


12.0 


15.13 


14.18 




9787.608 


14.75 


15.00 


15.42 


15.25 


11.8 


15.21 


13.78 


15.3 


9813.610 


14.73 


15.17 


15.30 


15.55 


12.5 


14.96 


14.13 


15.5 


9814.612 


14.82 


15.25 


15.10 


15.45 


12.5 


15.18 


14.39 


15.55 


9815.613 


14,81 


15,23 


14.60 


15.6 


12.6 


15.31 


14.39 


15.15 


9816.611 


14.88 


15. 32 


15.44 


15.3 


12.5 


14.95 


14.43 


14.6? 


30171.617 


15.12 


15.08 


15.42 


14.9 


11.6 


15.25 


14.49 




0172.615 


15.14 


15.11 


15.43 


15.6 


11,8 


15.0 


14.03 


15.05 


0519,606 


15.07 


15.15 


14.98 


15.3 


11.3 


14.74 


14.38 


15.7 


0520.606 


15.10 


15.05 


14.63 


15.6 


11.4 


15.10 


14.43 


14.95 


0550.608 


14.91 


15.10 


15.37 


15.35 


12.2 


14.80 


14.34 


15.4 


0553.604 


14.85 


15.26 


15.01 


15.35 




14.80 


13.92 


15.55 


0554.614 


14.76 


14.95 


14.35 


15.05 


11.2: 


14.76? 


13.96 


15.2 


0555.629 


14.84 


15.24 


15.40 


14.85 




15.0 


14.18 




0556.620 


14.93 


15.05 


15.40 


15.55 


11.3 


14.93 


14.30 


15.9 


0586.572 


14.95 


15.05 


15.18 


15.3 


11.3 


15.18 


13.96 


14.9 


0880.592 








15.25 








15.4 


.623 


14.70 


14.66 


14.65 


15.3 


10.7: 


14.8 


14.32 


15.0 


.659 


14.67 


14.57 


14.55 


15.5 


10.7: 


14.79 


14.40 




.690 


14.84 


14.88 


14.77 


15.4 


10.0: 


14.86 


14.31 




.730 


14.90 


14.95 


14.92 


15.6 


10.8 


14.85 


13.5 




.760 


15.07 


15.14 


15.10 


15.5 


10.8 


14.95 


13.7 




.788 










11.2 








0883.593 








15.5? 


11.4 






15.4? 


.630 


14.65 


14.66 


15.26 


15.3 


11.2 


14.78 


14.09 




.664 


14.80 


14.87 


15.41 


15.5 


11.3 


14.92 


14.27 


14.9 


0884.622 










11.3 








.680 


14.80 


14.78 


15.14 


15.5 


11.5 


15.20 


14.3 


15.15 


.721 


15.10 


15.06 


15.38 


15.3 


11.5 


15.31 


14.57 




.771 


15.15 


15.18 


15.40 


15.5 


11.6 


15.20 


14.47 


15.3 



33 

No. 79 No. 80 No. 81 No. 83 No. 84 No. 87 No. 92 No. 98 



30899.602 


14.74 


15.10 


14. 52 


15.5 


12.1 


15.17 


14.38 


15.25 


.647 


14.72 


15.15 


14.74 


15.3 


12.1 


15.15 


14.35 


15.1 


.701 


14.9 


15.12 


15.01 


15.55 


12.1 


15.25 


13.47 


14.95 


0900.604 


14.77 


15.07 


15.47 


15.5 


11.7 


15.04 


14.2 




.638 


14.88 


15.18 


15.42 






14.98 


13.5 




0901.676 


14.95 


15.35 


15.54 


15.4 




15.25 


14.29 


15.25 


0932.604 


14.55 


15.18 


15.15 


15.3 




14.87 


13.60 


15.3 


0933.589 


14.52 


14.87 


14.45 


14.95 






13.79 




1257.634 


15.00 


14.80 


15.34 


15.3 


11.1 


15.10 


14.12 


15.25 


1259.604 


15.20 


14.78 


14.47 


15.35 


11.4 


15.02 


14.37 


14.95 


1969.736 


14.63 


14.59 


14.81 


15.3 


11.3 


14.63 


13.57 


15.5 


1970.698 










11.6 








1976.641 


14.66 


14.96 


15.35 


15.05 


12.2 


15.00 


13.40 


15.15 


1977.690 


14.62 


14.75 


15.45 


14.9 


12.0 


15.27 


13.89 


15.3 


2000.641 


14.83 


14.79 


15.39 


15.4 


12.0 


15.21 


14.50 


15.55 


2004.652 


14.68 


14.65 


15.61 


15.5 


12.6 


14.95 


14.28 


15.6 


2006.599 


14.97 


14.66 


15.43 


15.3 


12.4 


14.71 


14.75 




2326.715 


14.73 


14.43 


15.40 


15.25 


12.1 


14.93 


14.17 


15.6 


2328.739 


14.60 


14.54 


15.71 


15.6 


10.7? 


14.90 


14.23 


15.6 


2354.604 


15.08 


14.83 


15.55 


14.9 


11.2 


14.95 


14.40 




2355.607 


15.06 


14.71 


15.53 


15.2 


10.9 


15.29 


14.37 


15.3 


2356.605 


15.17 


14.95 


15.29 


14.95 


10.8: 


14.83 


13.81 


15.4 


2357.604 


14.97 


14.97 


14.97 


15.5 


11.1 


15,03 


13.87 


15.6 


2361.704 


14.87 


14.65 


15.42 




11.3 


15.21 


13.99 




2734.604 


14.80 


14.75 


15.28 


14.9 


11.4 


15.21 


14.12 




2740.608 


14.59 


14.82 


15.13 


15.1 




14.73 


14.11 




2741.607 


14.85 


14.93 


15.19 


15.6 


12.4 


15.06 


14.34 


15.25 


2742.648 


14.66 




14.53 


15.6 


11.8 


15.0 


13.5 




2770.576 


14.66 


14.80 


14.95 


14.9 


11.9 


15.13 


14.18 




3068.668 


14.87 


14.98 


14.62 


15.35 




14.81 


14.35 




3069.654 


14.35 


14.92 


15.48 


15.3 


10.6: 


14.95 


14.08 




3095.604 


14.86 


15.13 


15.56 




10.7 


15.06 


14.47 




3096.609 


14.76 


15.17 


15.00 


15.2 


11.2 


14.81 


14.16 


15.55 


3476.602 






14.54 






14.93 


13.6 




3477.601 


15.02 


15.06 


15.71 


15.35 


11.3: 


14.80 


13.9 


14.95 


3481.597 


14.90 


14.95 


14.38 




11.7 


14.82 


14.32 




3505.572 


15.12 


14.98 


14.57 


15.2 


11.5 


15.05 


14.45 


15.3? 


3823.649 


14.41 


14.11 


15.33 






15.29 


13.96 




3858.636 


14.78 


14.45 


15.46 


15.3 


11.3 


14.64 


14.23 


15.55 


3860.589 


14.75 


14.97 


14.61 




12.0 


15.20 


14.41 




4180.634 


15.02 


15.16 


15.32 


15.4 


11.2 


14.92 


14.35 


15.25 


4181.607 


15.01 


15.15 


14.72 


15.3? 


10.8 


15.24 


14.30 


15.15 


4182.607 


14.82 


15.23 


15.41 


14.85 


10.9 


15.17 


14.24 


14.9 


4538.633 


14.89 


14.88 


15.35 




10.9 


14.83 


14.00 




4539.634 


14.84 


14.90 


15.37 


15.3 


10.9 


14.95 


13.80 


15.55 


4540.613 


14.78 


14.85 


15.12 






15.10 


13.98 




4572.602 


14.97 


15.02 


15.38 


15.05 


11.9 


15.08 


13.92 


15.15 


4573.635 


15.11 


15.17 


15.41 




12.3 


15.30 


14.47 




4574.602 


15.14 


15.05 


15.53 


15.4 


12.8 


15.45 


14.43 


15.6 



34 



Julian Day 


No. 79 


No. 80 


No. 81 


No. 83 


No. 84 


No. 87 


No. 92 


No. 


9f 


34575.603 


14.94 


14.87 


14.65 


15.25 




14.70 


14.35 






4929.623 


14.60 


15.05 


15.1 




10.8? 


14.80 


14.16 






5273.612 


15.22 


15.20 


15.5 


15.4 




15.09 


13.75 


15. 


05 


5274.609 


14.99 


14.91 


15.23 


15.6 


10.0: 


15.15 


13.95 






5275.610 


14.99 


15.10 


14.77 


15.3 


10.7 


14.55 


13.95 


15. 


55 


5307.600 


15.15 


15.06 


15.45 


15.15 


10.3: 


15.02 


14.28 






5308.599 


15.15 


14.91 


15.23 




11.3 


15.12 


14.36 






5309.600 


15.24 


15.08 


14.87 


15.15 


11.6 


14.92 


14.44 


15. 


7 


5310.600 


15.17 


14.90 


15.46 


15.15 


11.6 


15.04 


14.31 


15. 


3 


5658.601 








15.2 


12.0 










5661.602 


14.74 


15.01 


15.36 


14.75 


12.7 










5685.588 


14.95 


14.89 


15.55 


15.25 


12.2 


14.91 


13.70 






5687.592 


14.42 


14.93 


15.32 


14.7 




14.61 


14.10 






5688.590 


14.84 


14.85 


14.82 






14.89 


14.23 






6752.607 


14.58 


14.5 


15.35 


15.5 


11.9 


15.02 


14.26 


15. 


6 


6753.602 


14.59 


14.63 


15.00 


15.3 


12.5 


15.17 


14.24 


15. 


6 


7113.610 


14.73 


14.88 


14.95 


15.2 


12.2 


14.89 


14.32 


15. 


6 


7115.636 


14.72 


14.96 


15.44 


14.65 


11.8 


14.9 


13.50 


15. 


25 


7116.640 


14.82 


14.88 


15.38 




11.3 


14.99 


13.89 






8198.614 


14.89 


14.97 


14.50 


15.45 


10.5: 


14.99 


13.73 






8199.629 


14.73 


14.82 


15.35 






14.70 


13.81 






8584.628 


15.15 


15.13 


15.45 


15.35 


12.7 


15.07 


13.64 


15. 


5 


8586.605 


15.16 


15.27 


15.21 




12.4 


15.10 


14.27 






9262.779 


14.66 


14.91 


15.50 




11.6 


14.95 


14.47 






.785 


14.78 


14.82 


15.45 


15.3 


10.8: 


15.2 


14.38 






9265.680 


14.66 


14.73 


15.26 




11.5 


14.92 


14.38 






.684 










11. S 










.772 


14.72: 


15.16: 


14.93: 




11.6 


15.06: 


13.85 






.816 


14.80 


14.70 


14.54 


14.65 


11.0: 


15.07 


13.80 


15. 


5 


.819 


14.92 


14.89 


14.48 


14.7 


12.0 


15.20 


13.83 


15. 


55 


.847 


14.98 


14.81 


14.68 


14.9 


11.4 


15.00 


13.74 


15. 


6 


9270.772 


14.74 


15.04 


15.35 


14.8 


11.9 


15.00 


14.35 


15. 


7 


.776 


14.87 


14.87 


15.27 


14.5 


12.3 


15.10 


14.42 


15. 


4 


.798 


14.66 


15.02 


14.79 


14.55 




14.90 


14.21 






.803 


14.77 


15.12 


14.73 


14.6 


12.2 


15.12 


14.33 


14. 


9 


9271.615 


15.02 


14.66 


15.31 


15.4 




14.95 


14.28 


15. 


6 


.619 


15.21 


14.72 


15.53 


15.3 


12.5 


15.17 


14.36 


15. 


35 


.647 


14.97 


14.69 


15.29 


15.3 


11.4 


15.01 


14.23 


15. 


55 


.651 


15.00 


14.77 


15.36 


15.15 


12.5 


15.23 


14.35 


15. 


55 


.697 


14.80 


14.60 


15.32 


15. 5 




15.00 


14.07 






.701 


14.67 


14.89 


15.45 


15.3 


12.6 


15.07 


14.28 


15. 


15 


.722 


14.57 


14.72 


15.42 


15.4 


11.9 


15.01 


14.21 


15. 


25 


.725 


14.75 


15.11 


15.42 


15.15 


12.7 


15.18 


14.32 


14. 


95 


.771 


14.66 


15.11 


15.44 


15.3 




14.89 


14.26 


15 


2 


.776 










12.5 






14 


9 


.817 


14.85 


14.97 


15.42 


15.25 


11.5 


14.9 


13.85 


15 


1 


.820 


14.81 


15.02 


15.35 




12.4 


14.81 


13.87 







TABLE IV 
Photographic Magnitudes from Mount Wilson Plates 



36 



TABLE IV PHOTOGRAPHIC MAGNITUDES 



Plate Julian Day 



No. 1 No. 2 No. 3 No. 6 No. 7 No. 



No. 9 No. 10 No. 11 : 



3686P 


21338.885 


14.35 


15.45 


15.37 


15. 


15? 


15.32 


14.70 


14.63 


14.30 


15.33 




.887 


14.42 


15.40 


15.23 






15.30 


14.80 


14.73 


14.32 


15.02 


3694P 


21339.696 


15.53 


15.04 


15.04 


14. 


90 


15.68 


15.63 


15.23 


15.68 


14.85 




.699 


15.50 


14.98 


14.85 






15.67 


15.67 


15.17 


15.61 


14.67 


3696P 


.719 


15.53 


14.98 


14.98 






14.95 


15.80 


15.23 


15.87 


14.30 




.721 


15.60 


14.95 


14.95 






14.90 


15.68 


15.22 


15.65 


14.35 


3698P 


.740 


15.45 


15.02 


14.87 


14. 


75 


14.43 


15.67 


15.30 


15.62 


14.18 




,742 


15.67 


15.07 


14.90 






14.35 


15.62 


15.35 


15.65 


14.23 


3699P 


.765 


15.49 


15.18 


15.02 


14. 


8 


14.03 


15.60 


15.49 


15.57 


14.33 




.767 


15.63 


15.10 


14.93 






14.02 


15.71 


15.45 


15.76 


14.35 


3701P 


.787 


15.48 


15.35 


15.25 


14. 


9 


14.80 


15.55 


15.53 


15.60 


14.35 




.789 


15.51 


15.25 


15.14 






14.83 


15.70 


15.44 


15.66 


14.53 


3702P 


.807 


15.41 


15.39 


15.32 


14. 


8 


14.77 


15.78 


15.76 


15.63 


14.45 




.809 


15.48 




15.15 






14.87 


15.65 


15.77 


15.70 


14.65 


3704P 


.828 


15.75 


15.42 


15.09 


14 


85 


14.92 


15.62 


15.48 


15.65 


14.69 




.830 


15.55 


15.36 


15.10 






14.85 


15.55 


15.33 


15.65 


14.80 


3705P 


.848 


15.60 


15.47 


15.20 


14 


9 


14.97 


15.61 


15.43 


15.66 


14.97 




.850 


15.59 


15.42 


15.23 






15.06 


15.48 


15.42 


15.75 


15.02 


3707P 


.868 


15.45 


15.53 


15.18 


14. 


9 


15.17 


15.38 


15.42 




15.00 




.870 


15.47 


15.40 


15.09 






15.13 


15.24 


15.38 




14.97 


3708P 


.889 


15.35 


15.53 


15.42 


15 


05 


15.25 


14.98 


15.62 


15.85 


15.24 




.891 


15.55 


15.58 


15.57 






15.37 


15.01 


15.65 


15.95 


15.47 


3710P 


.910 


14.76 


15.76 


15.29 


15. 


05 


15.42 


14.55 


15.42 


15.65 


15.05 




.912 


14.82 


15.68 


15.25 






15.44 


14.55 


15.32 


15.58 


15.15 


3711P 


.932 


14.63 


15.62 


15.43 


15. 





15.50 


14.57 


15.50 


15.05 


15.01 




.934 


14.58 


15.51 


15.35 






15.45 


14.60 


15.39 


14.92 


15.21 


3713P 


.954 


14.75 


15.60 


15.43 


14. 


95 


15.55 


14.73 


15.48 


14.75 


15.20 




.956 


14.75 


15.52 


15.39 






15.40 


14.62 


15.35 


14.70 


15.34 


3714P 


.975 


14.85 


15.60 


15.48 


14. 


95 


15.60 


14.76 


15.55 


14.85 


15.35 




.977 


15.12 


15.52 


15.47 






15.54 


14.78 


15.56 


14.86 


15.45 


3716P 


.993 


14.93 


15.56 


15.48 


15. 


15? 


15.54 


14.87 


15.63 


14.99 


15.32 




.995 


15.06 


15.60 


15.50 






15.48 


14.79 


15.60 


14.99 


15.42 


3717P 


21340.010 


15.03 


15.60 


15.47 


15. 


25 


15.46 


14.92 


15.50 


14.90 


15.28 




.012 


15.14 


15.66 


15.57 






15.66 


14.94 


15.55 


15.00 


15.50 


3718P 


.015 


15.10 


15.37 


15.50 


15. 


25 


15.50 


15.20 


15.57 


15.17 


15.53 


3748P 


21375.679 


15.62? 


15.65 


15.50? 






15.65? 


15.85? 


15.85? 


15.35? 






.680 


15.56? 


15.37 


15.37? 






15.45? 


15.62? 


15.85? 


15.40? 


15.20 


3750P 


.695 


15.42 


15.53 


15.03 


15. 


5 


15.42 


15.53 


15.50 


15.31 


14.97 




.697 


15.55 


15.56 


15.05 






15.50 


15.52 


15.40 


15.30 


15.26 


3751P 


.718 


15.57 


15.65 


14.86 


15. 


15 


15.40 


15.29 


15.65 


15.92 


15.27 




.719 


15.63 


15.67 


14.90 






15.55 


15.39 


15.58 


15.90 


15.47 


3754P 


.766 


15.30 


15.64 


15.01 


15. 


3 


15.52 


15.47 


15.10 


15.78 


15.16 




.768 


15.36 


15.69 


14.93 






15.84 


15.40 


15.14 


16.00 


15.39 


3755P 


.790 


15.44 


15.60 


14.80 


14. 


95 


15.69 


15.76 


14.90 


15.75 


15.47 




.791 


15.35 


15.58 


14.85 






15.61 


15.61 


14.98 


15.84 


15.77 


3757P 


.807 


15.35 


15.35 


15.17 


15. 


15 


14.99 


15.57 


14.88 


16.00 


15.31 




.808 


15.57 


15.68 


15.03 






14.92 


15.50 


14.79 


16.00 


15.60 


3758P 


.827 
.828 








15. 


25 












3760P 


.845 


15.55 


15.72 


15.02 


15. 


15 


14.37 


15.28 


14.61 


15.81 


15.45 




.846 


15.57 


15.67 


15.07 






14.58 


15.23 


14.52 


16.05 


15.75 


3761P 


.862 


15.71 


15.55 


15.55 


15 


15 


14.89 


15.95 


15.13 


15.8 


15.47 



37 

FROM MOUNT WILSON PLATES 

^o. 12 No. 14 No. 15 No. 16 No. 18 No. 19 No. 20 No. 21 No. 25 No. 28 No. 29 No. 30 



5 


.70 


15.20 


15.00 


14.56 


14.67 


15.70 


14.93 


15.60 


14.50 


14 


43 


14.90 


15.50 


5 


.55 


15.20 


15.00 


14.65 


14.80 


15.75 


14.87 


15.75 


14.62 


14 


46 


14.91 


15.65 


5 


.53 


15.41 


15.41 


14.53 


15.63 


15.40 


15.53 


15.06 


14.55 


15 


68 


15.02 


15.60 


5 


.50 


15.40 


15.37 


14.40 


15.51 


15.40 


15.48 


14.87 


14.35 






14.80 


15.68 


5 


.87 


15.38 


15.25 




14.22 


15.56 


15.45 


15.22 


14.10 


15. 


64 


14.43 


15.66 


5 


73 


15.50: 


15.25 


14.60 


14.17 


15.48 


15.48 


15.19 


14.08 






14.38 


15.63 


5 


69 


15.32 


15.30 


14.85 


14.15 


15.69 


15.35 


15.17 


14.10 


15. 


71 


14.62 


15.45 


5 


52 


15.40 


15.32 


14.92 


14.17 


15.67 


15.10: 


15.28 


14.10 






14.63 


15.72 


5 


75 


15.41 


15.23 


14.96 


14.40 


15.63 


15.40 


15.40 


14.10 


15 


65 


14.90 


15.45 


5 


77 


15.45 


15.20 


14.97 


14.49 


15.90 


15.40 


15.35 


14.04 






14.86 


15.57 


5 


.83 


15.17 


15.30 


15.13 


14.80 


15.90 


15.44 


15.72 


14.16 


15. 


75 


15.08 


15.30 


5 


65 


15.17 


15.20 


14.98 


14.75 


15.83 


15.33 


15.58 


14.25 






15.10 


15.34 


5 


85 


15.50 


15.18 


15.26 


14.90 


16.05 


15.62 


15.62 


14.02 


15 


70 


15.25 


14.99 


5 


65 


15.40 


15.10 


15.00 


14.80 


16.00 


15.70 


15.69 


14.15 






15.24 


15.02 


5 


80 


15.35 


14.96 


15.03 


14.88 


15.80 


15.58 


15.40 


14.18 


15 


60 


15.25 


14.63 


5 


72 


15.40 


14.80 


14.88 


14.76 


15.80 


15.47 


15.20 


14.22 






15.25 


14.65 


5 


81 


15.42 


15.00 


15.05 


15.02 


15.72 


15.63 


15.40 


14.22 


15 


60 


15.38 


14.53 


5 


65 


15.48 


14.92 


15.15 


14.98 


15.65 


15.64 


15.31 


14. 19 






15.36 


14.60 


5 


65 


15.18 


15.02 


15.10 


15.10 


15.75 


15.51 


15.38 


14.32 


15 


65 


15.45 


14.65 


5 


45 


15.13 


15.00 


14.80 


14.80 


15.55 


15.50 


15.21 


14.22 






15.35 


14.63 


5 


81 


15.19 


15.19 


15.19 


15.40 


15.83 


15.60 


15.58 


14.27 


15, 


75 


15.57 


14.76 


5 


73 


15.34 


15.42 


15.15 


15.47 


15.83 


15.58 


15.65 


14.40 






15.54 


14.96 


5 


95 


14.90 


15.15 


15.33 


15.47 


15.82 


15.44: 


15.44 


14.30 


15. 


25 


15.71 


14.85 


5 


68 


15.00 


15.17 


15.13 


15.47 


15.76 


15.48 


15.37 


14.50 






15.68 


14.97 


5 


53 


14.77 




15.25 


15.53 


15.77 


14.90 


15.53 


14.36 


14 


79 


15.55 


14.95 


5 


39 


14.79 


15.42 


15.23 


15.55 


15.78 


14.81 


15.39 


14.39 






15.57 


15.00 


4 


73 


14.83 


15.38 


15.40 


15.67 


15.70 


14.65 


15.60 


14.43 


14, 


48 


15.66 


14.95 


4 


52 


14,67: 


15.25 


15.17 


15.57 


15.75 


14.64 


15.40 


14.38 






15.54 


14.95 


4 


44 


14.91 


15.44 


15.52 


15.74 


15.74 


14.55 


15.54 


14.42 


14 


60 


15.66 


15.09 


4 


30 


14.95 


15.45 


15.32 


15.59 


15.62 




15.41 


14.42 






15.56 


15.01 


4 


66 


14.97 


15.52 


15.34 


15.63 


15.26 


14.69 


15.53 


14.50 


14, 


75 


15.65 


15.08 


4 


50 


15.00 


15.45 


15.28 


15.72 


15.08 




15.50 


14.40 






15.65 


15.07 


4 


72 


14.98 


15.34 


15.25 


15.70 


14.25 


14.68 


15.53 


14.53 


14. 


77 


15.59 


15.08 


4 


97 


15.06 


15.40 


15.19 


15.72 


14.33 


14.70 


15.54 


14.52 






15.65 


15.18 


4 


80 


15.00 


15.45 


15.24 


15.57 


14.30 


14.67 


15.60 


14.57 


14. 


80 


15.30 


15.20 


5 


45? 


15.48? 


15.78? 


15.42? 


15.75? 


16.05? 


15.52? 


15.90? 


14.66 


15. 


85? 


15.66? 


15.40? 


5 


24? 


15.43? 


15.80? 


15.20? 


15.70? 


15.8? 






14.50 






15.57? 


15.30? 


5 


45 


15.19 


15.62 


15.37 


15.58 


15.73 


15.33 


15.40 


14.45 


15. 


51 


15.66 


15.35 


5 


31 


15.30 


15.52 


15.26 


15.60 


15.68 




15.26 


14.43 






15.68 


15.33 


5 


80 


15.37 


15.4 


15.27 


15.48 


15.02 


15.48 


15.69 




15 


34 


15.76 


15.27 


5 


60 


15.60 


15.31 


15.21 


15.55 


14.85 


15.37 


15.53 


14.99 






15.70 


15.36 


5 


75 


15.35 


15.50 


15.17 


15.62 


14.45 


15.58 


15.75 


13.75 


15. 


61 


15.64 


15.43 


5 


.85 


15.37 


15.29 


14.98 


15.81 


14.29 


15.62 


15.66 


13.87 






15.69 


15.33 


6 


05 


15.69 


15.24 


14.53 


15.76 


14.90 


15.72 


15.69 


13.80 


15. 


85 


15.30 


15.09 


5 


.97 


15.62 


15.07 


14.59 


15.84 


14.74 


15.77 


15. 18? 


14.07 






15.32 


15.10 


6 


.00 


15.44 


15.10 


14.60 


15.86 


14.88 


15.65 


16.00 


14.08 


15. 


35 


15.22 


15.31 


5 


.85 


15.57 


15.13 


14.29 
14.21 
13.95 


15.77 


14.92 


15.61 


15.77 


13.90 

14.12 






15.16 


15.10 


6 


.05 


15.39 


14.80 


13.80 




15.25 


15.72 


14.90 


14.32 


14. 


40 


14.64 


15.72 


5 


.87 


15.50 


14.66 


13.71 




15.05 


15.95: 


14.60 


14.18 






14.82 


15.52 


5 


.75 


15.67 




14.07 


15.95 


15.65 


15.47 


14.97 


14.20 


14. 


83 


14.47 


15.72 



38 

Plate Julian Day No. 1 No. 2 No. 3 No. 6 No. 7 No. 8 No. 9 No. 10 No. 11 

3761P 21375.863 15.85 15.34 14.95 14.48 15.85 14.92 16.0 15.45 

3763P .886 15.43 15.28 15.24 15.0 14.87 15.56 14.80 15.38 15.96 

.887 15.55 15.47 15.20 14.94 15.43 14.82 15.47 15.88 

3764P .905 14.50 15.68 15.35 14.9 15.35 15.62 14.85 15.70 15.62 

.907 14.81 15.53 15.22 15.40 15.62 14.91 15.62 15.48 

3766P .926 14.38 15.18 15.46 14.85 15.01 15.40 15.20 15.60 15.31 

.928 14.32 15.20 15.42 15.24 15.35 15.22 15.66 15.53 

3767P .946 14.31 15.03 15.40 14.75 15.13 15.09 15.12 15.50 

.948 14.38 14.97 15.45 15.23 15.01 15.26 15.66 

3849P 21435.746 15.45 15.62 14.82 14.65? 15.05 15.45 15.35 15.53 14.57 



Plate Julian Day No. 31 No. 32 No. 33 No. 34 No. 35 No. 38 No. 39 No. 40 No. 41 

3686P 21338.885 14.75 15.65 14.55 15.80 14.90 14.6 14.30 15.10 15.58 

.887 14.70 15.75 15.90 14.85 14.37 15.10 15.75 

3694P 21339.696 15.43 15.30 15.25 15.88 15.5 15.35 14.83 15.36 

.699 15.43 15.25 15.87 15.19 15.34 14.76 15.27 

3696P .719 15.40 15.43 15.3 15.25 14.90 15.5 15.40 14.90 15.53 

.721 15.32 15.51 15.22 15.43 14.90 15.48 



15.80 


14. 


90 


15.90 


14. 


85 


15.88 






15.87 


15. 


19 


15.25 


14. 


90 




15. 


22 


16.00 






15.88 


15. 


12 


15.95 






16.05 


14. 


85 


16.05 


14. 


80 


16.05 


14. 


77 



3698P .740 15.12 15.53 15.4 16.00 15.2 15.48 14.92 15.54 

.742 15.06 15.58 15.88 15.12: 15.50 14.95 15.64 

3699P .765 15.02 15.60 15.5 15.95 14.55 15.52 15.02 15.57 

.767 14.95 15.74 16.05 14.85 15.48 14.95 15.77 

3701P .787 14.97 15.83 15.5 16.05 14.80 14.55 15.57 15.12 15.82 

.789 15.00 15.80 16.05 14.77 15.50 15.04 15.62 

3702P .807 15.01 15.90 15.5 16.05 14.65 15.60 15.30 

.809 14.83 15.95 14.40 15.55 15.17 15.77 

3704P .828 14.86 15.72 14.9 14.70 14.7 15.48 15.06 15.70 

.830 14.75 15.72 14.60 15.51 15.06 15.62 

3705P .848 14.89 15.66 14.55 14.77 14.75 15.49 15.20 15.53 

.850 14.95 15.67 14.66 15.48 15.10 15.70 

3707P .868 15.00 15.61 14.45 14.80 15.05 15.57 15.15 15.70 

,870 14.96 15.55 14.62 15.42 15.07 15.56 

3708P .889 15.25 15.76 14.45 15.02 14.85 15.53 15.31 15.83 

.891 15.36 15.72 14.88 15.58 15.55 15.95 

3710P .910 15.32 15.70 14.6 15.10 14.9 15.66 15.35 15.82 

.912 15.24 15.62 14.99 15.60 15.20 15.76 

3711P .932 15.43 15.65 14.7 15.13 14.95 15.62 15.24 15.72 

.934 15.39 15.59 14.96 15.57 15.26 15.66 

3713P .954 15.38 15.73 14.95 15.09 15.05 15.57 15.19 15.73 

.956 15.30 15.66 15.04 15.47 15.07 15.68 

3714P .975 15.48 15.67 14.95 15.25 15.15 15.74 15.20 15.74^11 

.977 15.32 15.56 15.10 15.56 15.15 15.70 

3716P .993 15.35 15.26 14.95 15.35 15.5 15.63 15.00 15. 14 |ll 

.995 15.30 15.06 15.06 15.61 14.95 15.09 

3717P 21340.010 15.27 14.30 15.25 15.12 15.35 15.63 14.85 14. 59 |n 

.012 15.28 14.30 15.10 15.57 14.90 14.57 

3718P .015 15.32 14.25 15.35 15.26 15.28 15.05 15.40 15.12 14.60Jll, 

3748P 21375.679 15.60? 15.90? 15.32? 15.48? 15.48? 14.14?II2, 

.680 15.45? 15.70? 14.91? 15.37? 15.24? 14.17? 

3750P .695 15.45 15.37 15.3 15.05 15.2 15.32 15.07 14.30 

.697 15.44 15.37 14.95 15.40 15.12 14.29 

3751P .718 15.45 14.44 15.5 14.82 14.13 15.4 15.35 15.23 14.44 

.719 15.41 14.33 14.10 15.36 15.27 14.42 



39 



12 No. 


14 


No. 


1£ 


No 


16 


No. 


18 


No. 


19 


No. 20 


No. 


21 


No. 25 


No. 


28 


No. 


29 


No. 


3( 


5 15. 


53 






13. 


85 


16. 


05 


15. 


70 


15.40 


14. 


66 


14.09 






14. 


17 


15 


60 


5 15. 


67 


14. 


73 


14. 


22 


15. 


25 


15 


05 


15.19 


14 


50 


14.16 


14. 


55 


14. 


73 


15. 


19 


15 


70 


14. 


75 


14. 


15 


15. 


37 


15. 


60 


15.26 


14. 


46 


14.31 






14. 


65 


15 


26 


5 15. 


30 


15. 


15 


14 


46 


15. 


20 


15 


75 


15.03 


14. 


46 


14.35 


14. 


70 


14. 


70 


15 


30 


15. 


40 


15. 


09 


14. 


01 


15. 


35 


15. 


57 


14.96 


14 


65 


14.28 






14. 


85 


15. 


57 


3 15. 


11 


14. 


70 


14. 


55 


14. 


10 


15. 


76 


14.62 


14 


88 


14.65 


15, 


04 


15. 


13 


15. 


11 


5 15. 


15 


14. 


55 


14. 


20 


14. 


02 


15. 


75 


14.49 


14. 


55 


14.29 






15. 


06 


14. 


96 


5 14. 


81 


15. 


68 


14. 


47 


14. 


17 


15. 


91 


14.45 


14. 


92 


14.45 


15. 


12 


15. 


39 


14. 


95 


2 15. 


01 


15. 


60 


14. 


40 


14. 


20 


15. 


89 


14.40 


15. 


02 


14.45 






15. 


70 


14. 


88 


15. 


39 


14. 


91 


15. 


13 


15. 


75 


15. 


56 


14.89 


14. 


73 


14.43 


14. 


82 


15. 


41 


14 


96 



^o. 42 No. 43 No. 44 No. 45 No. 47 No. 52 No. 55 No. 58 No. 59 No. 61 No. 62 No. 63 



14.80 


15.10 


15.22 


15. 


15 


14.85 






15.53 


15.32 


15.50 


15.32 


14.64 


14.80 


14.95 


15.20 


15 


30 


14.97 


15 


00 


15.50 


15.27 


15.35 


15.20 


14.62 


15.32 


14.80 


14.90 






15.10 






15.28 


14.65 


15.10 


15.55 


15.58 


15.25 


14.72 


14.79 


14 


46 


15.20 


15 


67 


15.28 


14.67 


15.00 


15.62 


15.67 


15.28 


14.87 


14.56 






14.10 


15 


35: 


15.10 


14.83 


14.73 


15.50 


15.70 


15.27 


14.90 


14.55 


14 


40 


13.90 


15 


32 


15.10 


14.92 


14.68 


15.50 


15.65 


15.29 


14.75 


14.26 


14. 


09 


14.10 






15.30 


14.82 


14.53 


15.38 


15.69 


15.35 


14.96 


14.28 


14 


51 


14.05 


15 


45 


15.26 


14.93 


14.60 


15.27 


15.82 


15.37 


14.88 


14.23: 






14.20 






15.40 




14.75 


15.27 


15.72 


15.42 


14.93 


14.17 


14 


53 


14.30 


15 


28 


15.28 


14.95 


14.64 


14.90 


16.05 


15.32 


14.92: 


14.10: 






14.46 






15.72 




14.90 


15.04 


15.85 


15.36 


15.10 


14.23 


14. 


61 


14.65 


15 


26 


15.55 


15.15 


14.85 


15.07 


15.85 


15.45 


14.95 


14.05 






14.35 






15.72 




14.91 


14.77 


15.95 


15.35 


14.98 


14.20 


14. 


78 


14.26 


15 


18 


15.57 


15.20 


14.89 


14.95 


16.05 


15.49 


15.22 


14.58 


14. 


85 


14.63 






15.63 


15.40 


15.10 


14.90 


15.70 


15.40 


15.17 


14.65 


14. 


88 


14.66 


14 


85 


15. 55 


15.36 


15.10 


14.83 


15.80 


15.60 


15.27 


14.92 






14.66 






15.65 


15.27 


15.20 


15.00 


15.19 


15.53 


15.18 


14.77 


15. 


03 


14.76 


14. 


86 


15.60 


15.31 


15.20 


14.95 


15.31 


15.50 


15.00 


14.66 






14.80 






15.65 


15.07 


15.17 


15.05 


15.17 


15. 55 


14.83 


14.62 


14. 


83 


14.75 


14. 


80 


15.59 


15.25 


15.17 


14.98 


15.00 


15.67 


15.08 


14.96 






14.83 






15.73 


15.58 


15.31 


15.22 


14.85 


15.68 


15.17 


15.21 


15. 


51 


15.17 


14 


88 


15.75 


15.63 


15.50 


15.40 


15.03 


15.67 


14.79 


14.82 


15. 


06 


14.94 






15.85 


15.20 


15.40 


15.24 


14.30 


15.57 


14.80 


14.75 






14.97 


15. 


00 




15.35 


15.40 


15.32 


14.39 


15.53 


14.79 


14.75 






15.00 






15.82 


15.26 


15.38 


15.41 


14.54 


15.50 


14.75 


14.89 


15. 


12 


15.25 


15. 


01 


15.74 


15.32 


15.45 


15.51 


14.58 


15.57 


14.75 


14.87 






15.14 






15.78 


15.27 


15.45 


15.48 


14.65 


15.54 


14.74 


14.95 


15. 


26 


15.20 


15. 


18 


15.62 


15.38 


15.45 


15.45 


14.72 


15.62 




15.05 






15.30 






15.86 


15.34 


15.50 


15.40 


14.87 


15.61 


14.70 


15.12 


15. 


33 


15.09 


15. 


41 


15.77 


15.36 


15.47 


15.27 


14.89 


15.67 


14.69 


15.14 






15.35 






15.79 


15.19 


15.48 


15.34 


15.07 


15.70 


14.65 


15.04 


15. 


32 


15.39 


15. 


25 


15.79 


15.37 


15.60 


15.30 


14.97 


15.60 


14.92 


15.19 






15.15 






15.60 


15.52 


15.60 


15.18 


15.00 


15.69 


14.90 


15.23 


15. 


27 


15.34 


15. 


29 


15.60 


15.60 


15.57 


15.25 


15.06 


15. 55 


14.98 


15.06 


15. 


30 


15.17 


15. 


25 


15.49 


15.25 


15.37 


15.26 


15.17 


15.75? 


14.89? 














15.80? 




15.17? 


15.75? 


15.60 


15.70? 


14.92? 




15. 


15? 




15. 


20? 


15.56? 




15.16? 


15.70? 


15.40 


15.63 


14.80 


14.60 






15.20 






15.75 


15.10 


15.16 


15.49 


14.84 


15.56 


14.95 


14.65 


15. 


07 


15.25 


14. 


89 


15.55 




15.15 


15.52 


15.02 


15.63 


15.18 








14.86 






15.85 




15.33 


15.42 


14.52 


15.69 


15.17 


15.03 


15. 


43 


15.17 


14. 


88 


15.90 


15.53 


15.46 


15.47 


14.62 



40 



Plate 


Julian Day 


No. 31 


No. 32 


No. 33 


No. 


34 


No. 35 


No. 38 


No. 39 


No. 40 


3754P 


21375.766 


15.50 


14.57 


15.55 


14. 


71 




15.35 


15.53 


15.27 




.768 


15.33 


14.62 








14.90 




15.55 


15.31 


3755P 


.790 


15.44 


14.95 


15.4 


14. 


98 




15.3 


15.40 


15.10 




.791 


15.35 


14.98 








15.19 




15.35 


15.25 


3757P 


.807 


15.03 


14.91 


15.6 


15. 


06 




15.2 


15.40 


15.21 




.808 


14.95 


14.88 








14.98 




15.35 


15.30 


3758P 


.827 






15.25 








15.3 






3760P 


.845 


14.85 


15.17 


15.3 


14. 


90 




15.3 


15.57 


15.22 




.846 


14.75 


15.08 








14.70 




15.38 


15.23 


3 76 IP 


.862 


15.07 


15.35 


15.25 


15. 


35 




15.15 


15.75 


15.13 




.863 


14.72 


15.58 








14.40 




15.62 


14.91 


3763P 


.886 


14.85 


14.90 


15.25 


15. 


24 




15.3 


15.25 


14.73 




.887 


14.72 


15.07 








14.59 




15.26 


14.82 


3764P 


.905 


14.97 


15.66 


15.5 


15. 


10 




15.25 


15.86 


14.80 




.907 


15.03 


15.79 








14.82 




15.70 


14.71 


3766P 


.926 


15.23 


15.67 


15.2 


15. 


23 




15.4 


15.76 


15.05 




.928 


15.21 


15.85 








14.80 




15.69 


14.92 


3767P 


.946 


15.20 


15.82 


14.7 


15. 


27 




15.3 


15.85 


14.92 




.948 


15.37 


15.75 








14.91 




15.67 


15.01 


3849P 


21435.746 


15.03 


14.62 


14.95 


14. 


57 


15.07 


14.4 


15.25 


15.34 


Plate 


JuHan Day 


No. 64 


No. 65 


No. 66 


No 


67 


No. 68 


No. 69 


No. 70 


No. 71 


3686P 


21338.885 


15.45 


14.43 


15.20 


14 


5 


15.65 




15.70 


15.80 




.887 


15.25 


14.57 


15.12 






15.75 




15.50 


15.90 


3694P 


21339.696 


15.53 


15.38 


15.07 


15 


75? 


15.27 




14.85 


15.41 




.699 


15.52 


15.41 


14.93 






15.22 




14.67 


15.43 


3696P 


.719 


15.76 


15.65 


14.98 


15 


5 


15.15 


16.05 


14.62 


15.66 




.721 


15.67 


15.58 


15.02 






15.13 


15.87 


14.50 


15.57 


3698P 


.740 


15.69 


15.39 


15.01 


15 


35 


15.00 


14.93? 


14.70 


15.67 




.742 


15.62 


15.45 


14.92 






15.02 


14.88? 


14.80 


15.70 


3699P 


.765 


15.65 


15.45 


15.08 


15 


25 


15.33 


14.32 


15.11 


15.77 




.767 


15.75 


15.50 


15.02 






15.28 


14.26 


15.02 


16.00 


3701P 


.787 


15.87 


15.34 


15.15 


14. 


9 


15.22 


14.40 


15.20 


15.20 




.789 


15.62 


15.30 


15.13 






15.35 


14.49 


15.16 


15.16 


3702P 


.807 


15.74 


14.94 


15.58 


14 


55 


15.48 


14.90 


15.57 


15.57 




.809 


15.62 


15.07 


15.48 






15.61 


14.92 


15.53 


15.53 


3704P 


.828 


15.70 


14.70 


15.30 


14. 


45 


15.35 


14.76 


15.18 


15.18 




.830 


15.45 


14.77 


15.29 






15.22 


14.62 


15.22 


15.22 


3705P 


.848 


15.55 


14.90 


15.33 


14, 


55 


15.37 


14.87 


15.28 


15.28 




.850 


15.44 


14.90 


15.27 






15.44 


14.90 


15.27 


15.27 


3707P 


.868 


15.55 


14.53 


15.40 


14 


45 


15.58 


15.07 


15.30 


15.83 




.870 


15.35 


14.75 


15.37 






15.50 


14.89 


15.25 


15.72 


3708P 


.889 


15.58 


14.76 




14 


55 


15.85 


15.46 


15.71 


16.05 




.891 


15.60 


15.10 








15.75 


15.40 


15.72 


15.95 


3710P 


.910 


15.87 


15.20 


15.44 


14 


8 


15.58 


15.04 


15.34 


15.70 




.912 


15.69 


15.10 


15.47 






15.62 


15.15 


15.36 


15.70 


3711P 


.932 


15.76 


15.20 


15.52 


14 


9 


15.58 


15.47 


15.53 


15.25 




.934 


15.66 


15.25 


15.47 






15.57 


15.33 


15.58 


15.66 


3713P 


.954 


15.66 


15.28 


15.55 


15 





15.55 


15.63 


15.63 


15.73 




.956 


15.43 


15.00 


15.45 






15.50 


15.52 


15.54 


15.77 


3714P 


.975 


15.26 


15.40 


15.44 


15 


25 


15.65 


15.55 


15.53 


15.85 




.977 


15.05 


15.34 


15.45 






15.47 


15.45 


15.47 


15.76 


3716P 


.993 


14.74 


15.26 


15.28 


15 


25 


15.45 


15.60 


15.50 


15.70 



41 



No. 42 No. 43 No. 44 No. 45 No. 47 No. 52 No. 55 No. 58 No. 59 No. 61 No. 62 No. 63 



12.2 


15.25 


14.75 






14,95 


15,30 


15.83 




15.62 


15.19 


14.89 




15.14 


14.75 


14.75 


15.02 


15.17 


15.22 


15.95 


15.45 


15.69 


15.28 


15.08 


12.6 


15.09 


15.32 


15.35: 




15.17 




15.50 




15.72 


14.63 


14.93 




15.02 


15.42 


15.40: 


15.65 


15.33 


15,18 


15.50 


15.65 


15.76 


14.85 


15,13 


12.4 


14.91 




15.37 




15.26 




15.41 




15.73 


15.07 


15.21 




14.77 


15.16 


15.52 


15.49 


15.13 


15.30 


15.75 


15.75 


15.68 


14.83 


15.02 


12.4 




















14.40 




12.3 


15.00 


14.82 


15.45 


14.85 


14.00 




15.51 




15.79 


14.85 


15,06 




15.00 


14.90 


15.60 




13.92 


15.23 


15.61 


15.90 


15.90 


14.90 


15.08 


12.2 


15.13 


14.10 


15.35 




13.75 




15.80 




15.55 


15.55 


15.65 




14.85 


14.29 


15. 12 


14.05 


13.88 


15.45 


15.68 


15. 10 


15,30 


15.40 


15,49 


12.5 


15.25 


15.05 


16.05 


14.52 


13.93 




15.52 




15.85 


14.94 


15.10 




15.19 


15.15 


15.75 




14.07 


15. 10 


15.53 


15.63 


15.60 


15.10 


15.19 


12.4 


14.77 


15.41 


15.20 




13.72 




14.85 




16.05 


15.55 


15,48 




14.65 


15.13 


15.52 


14.30 


13.95 


15.62 


15,22 


15.53 


16.0 


15.31 


15,40 


12.3 


15.07 


14.40 


15.13 




14.57 




15.51 




15.53 


15.42 


15,60 




15.21 


14.39 


15.20 




14.52 


15.57 


15,42 


14.26 


15.75 


15.56 


15,78 


12.1 


15.12 


14.33 


15.07 




14.50 




14,78 




15.70 


15.68 


15,75 




15.20 


14.54 


15.23 


14.40 


14.62 


15.48 


14,60 


14.34 


15.69 


15.82 


15,90 


12.9 


15.28 


15.26 


15.23 


15.10 


15.07 




15.64: 


15.16 


15.68 


14.91 


15.42 


No. 73 


No. 74 


No. 75 


No. 76 


No. 77 


No. 78 


No. 79 


No. 80 


No, 81 


No. 83 


No, 87 


No. 92 


14.46 


13.62 


15.33 


15.33 


15.32 


15.15 


14.75 


15.07 




15.45 


15.15 




14.52 


13.55 


15.25 


15.23 


15.20 


15.10 


14.75 


15.13 


14.82 


15.43 


15.27 




15.03 


14.25 


15.03 


15,32 


15,35 


15.20 


15,03 






14.90 


15.23 


14.05 


15.00 


14.15 


15.08 


15.27 


15.37 


15.17 


14.92 


14.70 


15.45 


14.70 


15. 17 


14,00 


15.14 


14.16 


15.08 


15.23 


15.32 


15.03 


15.02 






14.70 


15.15 


14.01 


15.25 


14.13 


15.10 


15.28 


15.38 


15.02 


15.23 


14.45 


15.57 


14.82 


15.15 




15.30 


13.81 


15.08 


15.27 


15.35 


14.95 


14.87 






14.50 


15.25 


14.10 


15.38 


13.81 


15.18 


15.32 


15.45 


14.95 


14.96 


14.86 


15.52 


14.45 


15.45 




15.45 


13.60 


15.23 


15.28 


15.37 


14.90 








14.70 


15. 17 


14.22 


15.43 


13.63 


15.17 


15.35 


15.35 


14.83 


14.92 


14.92 


15.38 


14.62 


15.26 


14,18 


15.46 


13.85 


15.35 


15.32 


15.40 


15.00 


15.05 






14.75 


15.17 


14,25 


15.42 


13.85 


15.26 


15.32 


15.45 


14.97 




15.00 


15.30 


14.65 


15.11 


14,17 


15.57 


14.04 


15.37 


15.10 


15.57 


14.96 


14.74 






14.80 


14.96 


14,0 


15.57 


14.00 


15.30 


15. 17 


15.45 


15.05 


15,06 


15.05 


15.46 


14.80 


14.83 




15.35 


13.93 


14.89 


14.86 


15.36 


15.11 


15.05 






15.07 


14.70 


14,27 


15.30 


14.00 


15.12 


14.85 


15.30 


15.07 


14.95 


15.33 


15.33 


14.77 


14.80 


14.18 


15.30 


13.97 


15.19 


14.75 


15.19 


15.25 


14.91 






15.00 


14.65 


14,21 


15.25 


14.01 


15.23 


14.85 


15.39 


15.25 


14.89 


15.22 


15.31 


14.95 


14.85 


14.15 


15.12 


13.95 


15,25 


14.79 


15.24 


15.30 


14.67 






15.00 


14.74 


14.36 


15.05 


14.00 


15.17 


14.77 


15.28 


15.16 


14.75 


14.98 


15.30 


14,87 


14,75 


14.13 


14.98 


14.23 


15.42 


14.67 


15.13 


15.56 


14.70 






15,13 


14,71 


14.12 


15.20 


14.35 


15.38 


14.86 


15.38 


15.65 


14.92 


15,45 


15,25 


15.12 


15,08 


14.23 


14.98 


13.95 


15.37 


14,72 


15.10 


15,58 


14.57 






15.19 


14.76 


14.15 


14.95 


14.08 


15.42 


14.79 


15.15 


15,50 


14.80 


15.05 


14,95 




14.95 


14.30 


14.84 


14.18 


15.50 


14,69 


14.82 


15.43 


14,79 






15.27 


14.73 


14.20 


14.80 


14.22 


15.39? 


14,70 


14.89 


15.39 


14,58 


15.01 


14.43 




14.89 


14.20 


14.92 


14.21 


15.38 


14.59 


14.69 


15.30 


14,65 






15.36 


14.75 


14.23 


14.80 


14.19 


15.34 


14.58 


14,77 


15.32 


14,78 


14.96 


14.52 




14.85 


14.37 


14.79 


14.19 


15.42 


14.60 


14.65 


15.31 








15.29 


14.91 


14.10 


14.95 


14.25 


15.34 


14.57 


14,75 


15.32 


14.84 


14.90 


14.63 




14.98 




14.93 


14.25 


15.36 


14,65 


14,55 


15.17 


14.89 






15.39 


14.97 


14.10 



42 

Plate Julian Day No. 64 No. 65 No. 66 No. 67 No. 68 No. 69 No. 70 No. 71 No. 

3716P 21339.995 14.64 15.35 15.25 15.28 15.60 15.48 15.70 

3717P 21340.010 15,45 15.10 15.3 15.10 15.67 15.55 15.70 

.012 14.40 15.38 15.05 15.15 15.58 15.60 15.48 

3718P .015 14.52 15.23 15.35 15.5 15.10 15.65 15.75 15.47 

3748P 21375.679 15.73 15.70 14.9? 16.0? 15.80 15.90? 

.680 15.39 15.50 15.66? 15.54 15.80? 

3750P .695 15.51 15.73 15.65 15.05 15.65 16.00 15.80 15.13 

.697 15.47 15.65 15.60 15.70 16.00 15.85 15.15 

3751P .718 15.46 15.76 15.66 15.05 15.52 16.05 16.00 14.36 

.719 15.35 15.82 15.81 15.53 16.05 15.92 14.50 

3754P .766 15.75 15.64 15.12 14.55 15.12 15.85 15.79 14.50 

.768 15.59 15.45 14.96 15.05 16.05 15.95 14.41 

3755P .790 15.43 15.72 15.09 14.55 14.75 15.85 15.85 14.58 

.791 15.25 15.80 15.05 15.02 15.80 15.80 14.79 

3757P .807 15.35 15.84 15.03 14.5 15.40 16.05 16.05 15.31 

.808 15.35 15.60 15.13 15.35 16.05 15.95 15.30 

3758P .827 14.35 

3760P .845 15.67 15.75 14.85 14.45 14.93 15.65 15.55 15.22 

.846 15.53 15.45 14.90 14.79 15.83 15.50 15.08 

3761P .862 15.68 14.70 15.08 14.7 14.73 14.95 15.85 15.60 

.863 15.40 14.58 14.76 14.53 15.63 15.25 

3763P .886 15.70 14.35 14.95 15.1? 14.67 13.70 15.75 15.10 

.887 15.32 14.39 14.77 14.77 13.85 15.60 15.19 

3764P .905 15.85 14.45 14.67 15.15 14.90 13.90 15.95 16.00 

.907 15.53 14.65 15.02 15.21 13.85 15.62 15.67 

3766P .926 15.17 14.95 15.13 15.25 14.85 13.93 15.79 15.60 

.928 14.96 14.67 15.14 15.12 13.90 15.78 15.72 

3767P .946 14.56 14.53 15.30 15.25 15.60 14.53 15.97 16.15 

.948 14.59 14.62 15.30 15.64 14.45 15.82 16.0 

3849P 21435.746 15.41? 15.07 15.19 



43 



<io. 73 No. 74 No. 75 No. 76 No. 77 No. 78 No. 79 No. 80 No. 81 No. 83 No. 87 No. 92 



14.90 

14.85 

14.82 

15.20 

15. 15? 

14.93? 

14.88 

14.93 

il5.07 

115. 12 

115. 17 

115.40 

|l5.21 

15. 19 

!l5.50 

15.57 

il5.40 
115.32 
;i5.40 
115.17 



15. 
15. 



15 
19 



14.16 

14.24 

14.35 

14.40 

13.93? 

14. 10? 

13.88 

13.78 

13.79 

13.88 

13.75 

13.90 

13.60 

13.90 

14.05 



00 
17 



lis.oo 



15.28 



13.95 
14.01 
14.25 
14.15 
14.00 
14.18 
13.95 
13.88 
14.13 
14.17 
14.21 
14.25 
14.08 



15.42 

15.32 

15.32 

15.30 

15.66? 

15.50? 

15.42 

15.47 

15.40 

15.39 

15.50 

15.45 

15.43 

15.45 

15.65 

15.61 

15.47 
15.45 
15.80 
15.61 
15.15 
15.20 
15.02 
15.45 
15.18 
15.12 
15.17 
15.17 
15.20 



14.53 

14.53 

14.72 

14.60 

15.43? 

15.30? 

15.10 

15.12 

14.88 

15.04 

15.04 

15,00 

14.80 

14.94 

14.80 

14.75 

14.23 

14.77 

14.72 

14.78 

14.85 

14.51 

14.69 

14.85 

15.03 

15. 18 

15. 12 

15.18 

15.23 

15. 10 



14.60 

14.49 

14.63 

14.60 

14.88? 

14.91? 

14.89 

14.95 

14.84 

14.90 

15.01 

15.05 

14.90 

15.02 

15.25 

15. 10 

15.22 
15.17 
15.17 
15.10 
15.05 
15.03 
15.15 
15.35 
15.28 
15.42 
15.30 
15.41 
14.91 



15.05 

14.99 

15.05 

15.25 

15.52? 

15.32? 

15.15 

15.24 

15.16 

15.30 

14.75 

14.87 

14.98 

14.86 

14.88 

15.25 

15.00 
15.18 
15.60 
15.33 
15.44 
15.27 
15.20 
15.21 
15.25 
15.50 
15.27 
15.48 
15.28 



14.84 
15.02 
15.00 

14.87 



14.90 
15.00 
14.85 
14.90 
14.83 

14.70 

14.67 

14.54 
14.63 
15.23 



14.91 14.57 



14.94 
15.10 

14.70 

14.70 

14.85 

14.69 

15.22 

15.10 

15.23 

14.72 

15.56 

15.27 

14.83 

14.67 
15.16 



14.63 

14.82 

15.12? 

14.83 

14.57 

14.79 

15.02 

15.91 

15. 17 

15.53 

15.46 

15.70 

15.18 

15.33 
15.41 



15.37 

14.98 
14.69 
14.47 
14.95 
15.55 
15.35 

15.48 
15.29 
15.85 
16.05 
15.28 
15.52 
15.53 



15.11 
14.81 
14.98 
15.25 

15.70? 

15.25 

15.35 

14.89 

15.09 

15.25 

15.32 

15.25 

15.02 

15.21 

15.02 

15.05 
15.00 
15.84 
16.00 
14.87 
15.07 
15.21 
15.40 
15.35 
15.66 
15.33 
15.53 
15.05 



13.93 
14.06 
14. 15 
14.17 
14.32 
14.10 
14.35 
14.20 
14.07 
14.05 
13.43 
13.39 
13.52 
13.48 
13.59 
13.53 
13.77 
13.79 
13.80 
13.86 

14.00 
14.07 
14.0 

14.00 
14.02 
14.15 
14.02 
14.13 



44 



Christine M. Coutts and Helen Sawyer Hogg 



plates published by Bailey (1917) and from 81 by Oosterhoff (1941) 
were used to investigate the period changes of the RR Lyrae stars in 
M5. 

The reciprocal periods given by Oosterhoff (1941) were used in 
determining the light curves. The phases for the light curves were 
computed from the formula: 



phase 



Julian Date of Observation - 2400000 



Separate light curves were plotted for the following epochs: 1889, 
1895-96, 1897-99, 1901-02, 1904-05, 1908, 1912, 1917, 1934-35, 
1936-38, 1940-42, 1943-44, 1946-49, 1950-53, 1954-56, 1959-60, 
1963-64, 1966. Figure 5 shows the light curves of variable 7 at the 
various epochs. The light curve for each variable given by the 1934-35 
observations of Oosterhoff was drawn on tracing paper. Each was then 
fitted to the other curves by a horizontal shift. Thus the phase-shifts 
relative to the epoch 1934-35 were determined. (A positive phase-shift 
implies that the features on the light curve in question occur at later 





- 












1889- 


150 


- 












- 


14-5 


•.•• 












95 
96- 


155 


- 












. ; - 


14-5 


-. 












97 

98- 

99 


155 


- 










• 


- 


14-5 


-. 












1901 " 
02 _ 


15-5 


- 












■- 


145 


- 












04 
05 
08_ 


155 


- 














145 














12 - 




- 


• _ 






_ 




- 


Wt 


_ 








■ 




_ 
















17 


14-5 


_ 




, 


■-•. 






,: 


155 


- 














14-5 


- 












34 
35 


155 


- 


"'w-c 


.• ..'«5.:-.s. . .... 




•■■•-w. 


.r.-.y, -. 


- 



15 5- 
14 5- 

155 

145 



155 
145 

15-5- 



14 5- 
155- 



47 - 
48 
49 - 



Fig. 5 — Illustration of light curves for determination of phase-shift diagram 
(variable 7). 



Period Changes of RR Lyrae Variables in M5 



45 



HARVARD 
1895 



MT. WILSON DAVID DUNLAP 

1917 ,1937 I 1966 



HARVARD 
1895 



-10 

-10 



•10 

-10 

•50 

•30 

•10 

-10 

■20 



■10 



1934 1943 



A PHASE 
50 



I I I — I — I — I — I — 1 — I — I — I — r 



MT. WILSON DAVID DUNLAP 

1917 1 1937 I 1966 

Z"' 1934 1943 ^ 



T — I r-r 



FiG. 6 — Phase-shift diagrams (phase-shift in fraction of a period). 

phases than on the 1934-35 curve.) Then a phase-shift diagram was 
plotted. 

No phase-shift diagrams were plotted for variables 2, 14, 18, 25, 35, 
44, 52, 58, 65, 66, 67, 68, 72, and 92 because their light curves were too 
irregular. The phase-shifts for tiie other 52 stars are listed in Table II 
and their phase-shift diagrams are shown in figure 6. 



46 



Christine M. Coutts and Helen Sawyer Hogg 



HARVARD 
1895 



MT WILSON DAVID DUNLAP 

1917 ,1937 I 1966 



1912 ' 
— I — r 



1934' 1943 

M.I 



HARVARD MT WILSON DAVID DUNLAP 

1895 I 1917 |I937 , 1966 

' 1912 ' 1934! 1943 '" 



a PHASE 
-10 

-10 



•10 

- 10 
•10 

- 10 



I I I I — I — I — I — I — I — I — I — I — I — I — I — 1 — I 

1890 1905 1920 1935 1950 1965 



— 1 1 — I 1 — I 1 1 — I 1 — I 1 — I 1 1 1 1 1 

1890 1905 1920 1935 1950 1965 



Fig. 6 — Phase-shift diagrams (continued). 



Determination of Period Changes 

The changes of period have been determined in two ways: by 
fitting parabolas to the points on the phase-shift diagrams to determine 
the rate of period change, jS, and by fitting intersecting straight hnes to 
the points to determine the amount of period change, AP. 

Standard parabolas were plotted on transparent paper for 11 values 



Period Changes of RR Lyrae Variables in Mo 



47 



HARVARD 
1895 



-20 

10 
-10 
•80 
•60 
•40 
•20 
O 
-20 



MT WILSON DAVID DUNLAP 

1917 [1937, 1966 



HARVARD 
1895 



MX WILSON DAVID DUNLAP 

1917 ,1937 I 1966 



— I — I — I — I — I — I — I — I — I — I — r 

1905 1920 1935 1950 



0- 



20- 
0- 

10- 
-10- 



1934! 1943 




1950 1965 



Fig. G — Phase-shift diagrams (continued). 

of /3/2P2 between IQ-i" and IQ-^ days-^. These were fitted visually to 
the phase-shift diagrams and the values of ^ computed for each star 
from tlie most suitable paraljola. Most of the phase-shift diagrams are 
not true parabolas and there is an uncertainty of about 2") per cent in 
the values of /3. 



48 



Christine M. Coutts and Helen Sawyer Hogg 



+ .30 


















+ .20 


- 






" X 


• 








+ .10 

.00 

- .10 


- 


• ..• 


• 


• 
• 

• •• 


• 
• • 


• 




• 


- 


*• 




••• . 

• • 








- .20 


- 






• 


• 








-.30 


- 








X 








-.40 


1 


• 
1 




1 


1 


1 




1 r 



Fig. 



.2 .3 .4 .5 .6 .7 .8 .9 

-The rate of change of period, /3 (in days per million years) determined 



from fitting parabolas to the points in the phase-shift diagrams, plotted against the 
period (in da\,s), stars with constant period included. 

An attempt was made to determine the amotint of tliis change in a 
million >ears in order to compare with the values of ^ determined from 
the paral)olas. (3f the 50 stars for which the period increased, decreased 
or remained constant during the seventy-year interval, periods of 18 
(or about one-third) remained constant. Then, if the interval of 
observations was extended to 100 years, it miglit be expected that 
abrupt changes in the periods of these stars would be observed, i.e., a 
star changes its period abruptly about once in 100 years. At this rate, 
in a million years, the period of a star would change by 10,000 times 
the amount observ^ed in 70 years. Assuming this, the period change 
expected in a million years is calculated for those stars for which 
changes were observed in the present investigation. These are listed in 
Table V and plotted against period in figure 8. 

If the phase-shift diagram produced a single straight line, the 
period weis assumed constant and corrected if necessary: AP (correc- 
tion to period) = slope X P^. These corrected periods are listed in Table 
V. The light curves for these stars are shown in figure 9. 

In Table V the epochs are those given by Oosterhoff in heliocentric 
Julian days with the first two digits (24) omitted. Successive columns 
give the period, reciprocal period, /3 (the rate of change of period in 
days per million years), and the projected period change for a million 
years (assuming the period changes abruptly). The periods adopted 
here are those computed from Oosterhoff 's reciprocal periods. It was 
found in the course of this investigation that Oosterhofif's periods do 
not ahvays correspond to his reciprocals. Besides the stars with period 



Period Changes oj KR Lyrae Variables in Mo 



49 



TABLE V 
Periods of Variables in M5 



Var. 



Epoch from 
Oosterhoff 



Period 
days 



Reciprocal 
Period 



j3 davs/ 
106 ^.j- 



Rate 
abrupt 
change 



Notes 



1 


27563.794 


0.5217856 


1.916496 






const. 


2 


27601 . 700 


0.526 








1 


3 


27567.842 


0.6001832 


1.666158 


.039 


.044 




4 


27627.708 


0.4496402 


2.224006 


.234: 




15 


6 


27567.856 


0.5488311 


1.822054 


-.048 


-.026 




7 


27601.730 


0.4943896 


2 . 0226962 


.105 


.100 




8 


27605.697 


0.54623 


1 . 83075 


.091 


.077 




9 


27653:855 


().G9S8950 


1.43083 






const. 


10 


27567.825 


0.r):3()6628 


1 . 8844359 


-.020 


-.037 




11 


27563.817 


0.5958914 


1.678158 






const 


12 


27601 . 762 


0.4677144 


2.138057 


-.064 


-.096 




13 


27567 . 800 


0.5131223 


1.948853 


.038 


.046 




14 


27567 . 974 


0.4872423 


2.052367 






1 


15 


27567.908 


0.3367607 


2.969468 


.050 


.084 




16 


27567.781 


0.6476223 


1.54411 


.124 


.069 




18 


27567 . 773 


0.464 


2. 15573 






1 


19 


27601.706 


0.4699535 


2.12787 




.374 


2 


20 


27601 . 729 


0.60i»4759 


1 . 640754 






const 


21 


27605.684 


0.G04S941 


1.653182 






const 


24 


27567.821 


0.4783771 


2.090401 


.205 




15 


25 


27567.766 


0.508 


1.969 






3 


26 


27601.761 


0.6225642 


1.60626 


.044 




15 


27 


27888.894 


0.4703 


2.126217 






4 


28 


27540.882 


0.5439474 


1.838413 


- . 127 


-.292 


5 


29 


27567.700 


0.4514355 


2.215166 


- . 120 


-.180 


6 


30 


27567.761 


0.r)i)21755 


1.6886886 






const 


31 


27567.872 


0. 3005826 


3.326S725 






const 


32 


27605.754 


0.4577SG3 


2.1844254 






const 


33 


27601 . 738 


0.5014722 


1.9941286 


.037 


.041 


7 


34 


27567 . 727 


0.5681431 


1.76012 






const 


35 


27567.866 


0.3081197 


3.245492 






1 


36 


27563 . 868 


0.6277229 


1 . 5930596 






const 


37 


27605.762 


0.4887941 


2.045851 


-.039 




15 


38 


27889.937 


0.4704441 


2.1256511 








39 


27563.832 


0.5890346 


1.697693 


.051 


.035 




40 


27605.698 


0.3173286 


3.1513078 


.029 


.015 




41 


27567.879 


0.4885749 


2.046769 


-.070 


-.072 




43 


27601.767 


0.6602264 


1.514632 






const 


44 


27601.732 


0.329 


3.0362 






10 


45 


27567.774 


0.6166364 


1.6217012 






const 


47 


27563.861 


0.5397295 


1.85278 


-.085 


-.077 




52 


27563.804 


0.5017848 


1.992886 






1 


55 


27601.734 


0.3288968 


3.040467 


.032 


.028 




56 


27889.931 


0.5346903 


1.8702415 


-.264 




15 


58 


27601.716 


0.491265 


2.03556 






1 


59 


27540.936 


0.5420259 


1 . 8449303 






const 


61 


27567.826 


0.5686157 


1 . 758657 


.095 


.107 




62 


27601 . 704 


0.2814092 


3.553544 




.193 


11 


63 


27567.851 


0.4976763 


2.009338 


.037 


.031 




64 


27540.853 


0.5445075 


1.836522 


-.127 


-.117 




65 


27628 . 729 


(t. ISOGOI 


2 . 08034 






12 


66 


27567.813 


0. ;!.")( )G81 


2.85159 






13 


67 


27567.733 


0.3490462 


2.86495 






13 



50 



Christine AI. Coiitts and Helen Sawyer Hogg 
TABLE V — continued 













Rate for 






Epoch from 




Reciprocal 


/3 days 


abrupt 




Var. 


Oosterhoff 


Period 


Period 


10« yr 


change 


Notes 


68 


27628.727 


0.3342797 


2.991507 






13 


69 


27567.761 


0.4948743 


2.0207151 






const. 


70 


27567.930 


0.5585255 


1.7904286 


.184 


.268 




71 


27541.011 


0.5024676 


1.990178 


.073 


.039 




72 


27596.82 


0.562 


1.779 






1 


73 


27601.753 


0.3401118 


2.94021 


.050 


.074 




74 


27626.684 


0.4539961 


2 . 202662 


-.060 


-.048 




75 


27596.816 


0.6854136 


1.458973 


.070 


.057 




76 


27563.813 


0.4324210 


2.312561 


.027 


.118 




77 


27605.721 


0.8451121 


1 . 183275 


.106 


.176 




78 


27567 . 727 


0.2648174 


3.776187 






const. 


79 


27567.884 


0.3331387 


3.001753 






const. 


80 


27562.986 


0.3365424 


2.9713936 


-.017 


-.014 




81 


27567.972 


. 5573235 


1 . 79429 


-.184 


-.265 




83 


27567.783 


0.5533073 


1.807314 






const. 


87 


27540.914 


0.7383888 


1.3543 






const. 


90 


27540.828 


. 557 1 527 


1 . 79484 


.076 




15 


92 


27567.963 


0.4635789 


2.15713 






14 


98 


27605.737 


0.3063857 


3.26386 


-.416 


-.060 





Notes 



3. 



4. 



8. 



10. 



11. 



12. 

13. 
14. 
15. 



Irregular; therefore no phase-shift diagram was plotted. 

No parabola could be fitted on the phase-shift diagram. Period changes abruptly 
between 1945 and 1950. 

P^oUowing component of close double. Of Oosterhoft's two possible periods, 
0.508 and 0.517 days, the D.D.O. observations fit the former, but not well 
enough for a phase-shift diagram. 

Irregular, Oosterhoff. A complicated phase-shift diagram indicates a fluctuating 
period. 

Period change calculated from difference in slope between first and third line of 
three straight lines. 

Oosterhoff found the shape of the light curves abnormal for the period, with 
rising branch less steep than expected. 

\'isual observations by Barnard (1909). His published Julian Dates appear to 
be calculated for noon C.S.T. On this assumption, his light curves coincide with 
those of Bailey (1917). 

Irregular Oosterhoff', and current investigation. Bailey class c, and no phase- 
shift diagram made. 

Phase of light curve in 1917 ambiguous with respect to the others, which prevents 
definite determination of period change. 

Period irregular. The D.D.O. observations fit Oosterhoft's longer period of 0.329 
better than his 0.247-day period. 

Positions of light curves from observations of Bailey in 1912 and Shapley in 
1917 ambiguous, relative to other years. Net change in period calculated from 
slope of line representing Bailey's observ^ations and that for D.D.O. observations. 
Probably not irregular, but because of uncertainties in measures due to closeness 
to another star no phase-shift diagram was constructed. 
Bailey class c, some irregularity, no phase-shift diagram. 
Measures difficult on D.D.O. plates; perhaps irregular. 
/3 determined by Oosterhoff. 



Period Changes of RR Lyrae Variables in Mo 



51 



changes, the tal)le hsts those with constant or irregular periods, and 
six stars for which Oosterhoff (1941) found period clianges, but which 
were not studied on the David Dunlap plates. 

Discussion 

From this study of the variables in Mo A\"ith observations over an 
interval of 75 years, we have found that for 18 stars the periods are 
constant, for 20 t\\e\ have increased, and for 12 they have decreased. 



-1- .40 


- 






• 






-1- .30 


- 






• 






-f .20 




• 








• 


+ .10 


- 


% 




• 






.00 
- .10 




. .'^ 




*• 






- 


• 


• 


• •* 






- .20 


. 












- .30 


- 






• 

• 







■2 .3 .4 .5 .6 .7 .8 .9 

Fig. 8 — The projected period change (in da^s per million years) determined from 
fitting straight lines to the points in the phase-shift diagrams, including stars with 
constant period. 



For the other 16 stars, periods are not well determined or are irregular. 
The median rate of change of period for the stars with increasing periods 
is 0.05 (±0.02) days per million years; the median rate for those 
decreasing is 0.075 (±0.02) days per million years. The median rate of 
change of periods of all the stars considered together is zero. It is 
interesting to try to determine if these changes are due to evolution of 
the stars across the horizontal brancli of the H-R diagram or if they are 
just random. If the former, then it follows that both the decreases and 
the increases must have evolutionary significance. Otherwise, since the 
median rate of period change is zero, the changes do not indicate an 
evolutionary trend. 

Sandage (1957) has calculated, by semi-empirical methods, a time 
scale for stars in the RR Lyrae phase in M3. According to him, the 
stars spend 8 X 10" ^ears in the RR Lyrae stage. The H-R diagram 
for M5 is very similar to that of M3, and so, it might be concluded that 
stars in M5 also spend al)out 8 X 10^ years in the RR Lyrae stage. 
According to figure 10, the range of periods an RR Lyrae star in M5 



52 



Christine M. Coutts and Helen Sawyer Hogg 



145 
15-5 











^ 












- 








^ 


■V 


'•i: '. ' 






- 










































1 


■iiviry-: 


'■y- 








■ 


1 


..•••)■• 


"'- 



0-5 



145 
15-5 



0-5 















.'jS^Tu: . 










II 






































•';■ <^*-. 


s ••:. 








~ 
















■-^.c--- 








- 


-^"7 


>>?•. 


■r^ 


f: 


^ 


;? 


1 


• '.-*■ 


"*: 




ifi'V 


*• 



0-5 



05 



14-5 
15-5 



0-5 




05 



14 5 
15-5 



05 



'^'^-i'-.-.'.j:: 






0-5 



_ 




















31 








5>.'- . ■• 


•'■?' 


•>o 














•%■»??. 


yVi 






1 




■■■'•■^ ^i 




^5? 


t-**- 



05 









••"?i 




32 










^k:.. . 




1 


iHihSi-ji 


•^; 


• 1 


■■^% 





0-5 



Kfi 










:■ 


K- 








20_ 






.* 










'7:'r-.i*>. 


V 


.. 




15-5 


rf< 


^■^.•' 


:^ 


Tr: 










1 


ft? •"• 



05 



05 























21 


14-5 










v:: 


'V""!-..- 










15-5 


1 


r!: 


•5/ 


:'r-'^:- 


\"V 


1 


• ■:•*:• 


■ST 


1 


•Vj-ii- 



145 


_ 








^^ 












34 _ 


155 


-?. 


■*:^l'. 


.*. 


'"■••i" 


1 




■;•*. 


=t 


ij? 


1 


if^i 



05 



05 







..-.•!• 






36 


-• 




• ■*■ 1 '„•• .-■■■ '" 






. . . ~ 


- . 


."■ ■ :. 


;'• v=*:-"V 


•'.■■■••*■ .'■'•"■^••' 




•.:' •- ■ - 






. -i^ : '■ 


• "■ • « "1 


:.;.»•:■■ 


."- .• 




■ ■_:•: 


1 




1 





14-5 

15-51- 

I 

05 05 05 05 

Fig. y — Light curves for stars with constant periods. 

may take is 0.55 days (allowing for a gap between types c and a). Thus 
the expected average rate of change in period is 0.007 days per million 
3'ears. The minimum rate that can be detected over 75 years depends 
on the period. The mininumi value of (3/'2P^ observable at the present 
time is 10"^" days"-. Tliis corresponds to the following values for (3: 

(3 = 0.04 days per million years for P = 0.8 days, 
= 0.02 days per million years for P = 0.5, 
= 0.005 days per million years for P = 0.25. 



Period Changes of RR Lyrae Variables in Mo 



53 



145 








43 


155 


1 1 


" ""-i-?*^!" 


1 


-iP'lr 



05 



0-5 



14 5 
155 









45 


-; ••.■.. 


■ =•!:.>>■■ 


■Vi":s^^-:^,. .- 


'""••.•■■••:'••:" 


i" 




1 


l" 



05 



05 



145 
155 





-■<••■ ■ • 




59 




'X '■ ■="; 


"v- 




hi¥^-^ 


'f. 


.■'•.'-:_"E!. 


^i.r;fd_ 


1 


1 




- 





05 







05 








^:. 


69 


14-5 


- 




.••'•>:• 


■.. ■■:■■., . 


15-5 


^^• • •■ 

1 


':»»!i-^ 


1 


1 



05 



0-5 















78 


4b 


- 














_... 


,.i;>^"?;' 


•••:>■■' 


'^■■'■■k:-: 








~A ■••'•^i^-'" 










''<.->-; ^-.t^:- 


5 5 


1 










1 



05 



05 



145- 
155 






05 



05 



145 


- 




!.i^'^-. 




83 


155 


'■■f-\ 

1 


,:-.i;:..-H 


1 


••••^i^^f^'i •"": 


1 





05 











05 














87 


4-5 


- 






-■-ii^HiV^-:,:.: 




- 




:'iv.' • 


1 •"■ '•; 


■^ 


. :] " * ■•'•.* " ■*• 




■H*:: ..'■-•-. I. >. -.-.;'" 


55 


1 






1 




1 



05 



05 



Fig. 9 — Light curves for stars with constant periods (continued). 

Thus, using the present observations, onh- for variables with 
periods < 0.8 days is it possible to detect evolutionary- changes in 
period. Almost all the variables in ^Ib have periods greater than 0.3 
day. However, Sandage's computations have been made on the 
assumption that stars cross the RR Lyrae gap only once and in the 
direction of decreasing periods, whereas the periods of the stars in Mo 
exhibit both increases and decreases. 

Theoretical calculations of Faulkner and I ben (196G) indicate that 
stars do change direction of evolution on the horizontal branch. They 
have considered models with two different hydrogen compositions in 
the envelope: X ^ = 0.90 and A'^ = 0.65. These models have double 
energy sources: lielium l)urning in the core and hydrogen burning in a 
shell outside. In the models witli A", = 0.90, the helium burning in the 



54 



Christine M. Coutts and Helen Sawyer Hogg 



20 
IS 


- 








H 


1 


10 








5 


\- 








n 




1 


1 


1 , , 1 1 



.3 .4 .5 .6 .7 8 

Fig. 10 — Period-frequency diagram for Mo. 



core dominates the energ^• production and the stars move to the right 
in the H-R diagram (analogous to stars moving off the main sequence). 
Then, when the core is exhausted and gravitational contraction sets in, 
the star moves to the left in the diagram, but much faster. The 
favoured model with this composition spends about 4 X 10^ years 
crossing the horizontal branch (about 1.3 X 10^ years as an RR Lyrae 
variable) corresponding to an average increase of period at the rate of 
0.04(2) doxs per million years followed by decrease of period at a 
faster rate. On the other hand, in their models with X^ = 0.65, the 
hydrogen burning in the shell dominates the energy- production and 
there is a resulting contraction in the envelope to maintain a high 
temperature and density in the shell, causing evolution to the blue in 
the H-R diagram. When a point is reached where Iielium l)urning in 
the core dominates the energy production, the star evolves to the red 
at a much faster rate. In the model favoured by Faulkner and I ben 
(1966) with this hydrogen envelope composition, the star spends 
1.3 X 10^ years on the horizontal branch evolving to the blue (about 
4 X 10" years in the RR Lyrae stage). This would indicate an average 
decrease of period of 0.014 da>"s per million years followed by an 
increase at a faster rate. This rate of decrease is below the limit of 
detection for periods greater than 0.4 days, and most of the decreases 
are observed at periods greater than this value. 

In the case of the models with Xe — 0.90, the average increase of 
periods at the rate of 0.042 days per million years predicted by the 
theory is approximately what is observed, but the observed decreases 
are at the same rate, and not faster as expected from the theory. 

It therefore seems likely that the observed period changes are not 
caused by the evolution of the stars across the H-R diagram. 

Furthermore, Sandage (1965) has pointed out that if the RR Lyrae 
stars follow evolutionary tracks like those of Faulkner and I ben (1966), 



Period Changes of RR Lyrae VariahJes in Mo 55 

then there would be a correlation between the rate of period change 
and the mean magnitude of the RR L^•rae stars. All the stars with 
decreasing periods would be brighter or fainter than those with 
increasing periods. An examination of 26 stars in A 1 3, using period 
changes determined by Szeidl (1965) and mean mpg and nipy colours 
determined by Roberts and Sandage (1955), does not indicate any 
correlation between period changes and mean magnitudes, nor does an 
examination of 14 stars in co Centauri, ^\ith the period changes 
determined by Belserene (1964) and mean B, 1' magnitudes of Dickens 
and Saunders (1965). However, these are very small samples. 

An explanation for ol)served period changes based on evolution also 
seems difficult l)ecause tlie patterns of observed period changes differ 
from cluster to cluster. In a; Centauri, there is a predominance of 
variables with increasing periods, while in M3, there are equal numbers 
increasing and decreasing, and aliout half of the stars investigated 
show irregular period changes. In M15 and M5, a significant proportion 
of the stars investigated have periods which have remained constant 
throughout the years of investigation. (Light curves for the variables 
in M5 with constant periods are shown in figure 9.) 

In the case of a variable whose period appears constant, it is possible 
that the period is changing at a rate too slow to be detected, or that, if 
the change is abrupt, it lias not occurred in the observed time interval. 
Assuming that the periods of the stars in M5 change abruptly, the 
period changes so determined are shown plotted against the values of 
j8 determined from the assumption that the period varies at a constant 
rate. With the exception of variable 98 (with an unreliable /?), the 
points define a straight line with a slope slightly greater than unity 
(about 1.2) which seems to justit\- the determination of rates of period 
change by fitting intersecting straight lines to the diagram. This is 
useful because many of the phase-shift diagrams (that of variable 19 
in particular) resemble straight lines more than parabolas. 

It is important to determine whether or not the period changes are 
abrupt, because our interpretation of the ol)served constancy of period 
for some of the stars depends on this. To do this, we must accumulate 
observations for another 30 years and then plot new phase-shift 
diagrams for the stars which appear to have constant periods at the 
present time. If they do exhibit period changes, it will not be justified 
to consider them as variables witli constant periods with regard to 
.evolution. 

Also we might arrive at tlie most suital)le interpretation of the 



56 



Christine M. Contts and Helen Sawyer Hogg 



+.20 



+.10 



-.10 



-.20- 



-.30 




-.40 -.30 -.20 -.10 



+ .10 +.20 



Fig. 11 — Projected period changes (days per million years) versus (in days per 
million jears). 



diagrams by reinvestigating tiie stars with observed period changes. If 
the diagram is a parabola, then as different periods are tried, the para- 
bola should retain its shape, but the position of the vertex should shift 
so that it occurs on the time axis at the point where the assumed 
period is actually the true period. If the diagram is best represented by 
two intersecting straight lines, then the point of intersection should 
always occur at the same time, as different periods are tested. The 
slopes of the lines would change, but the difference in slope should 
remain constant. This method is now being explored at the Asiago 
Astrophysical Observatory for some of the stars in Mo. Before the 
possible evolutionary interpretations of the period changes observed in 
the different clusters can be considered, it is important that the signifi- 
cance of the apparent constancy of period for some of the stars be 
understood. 

A very important point illustrated by this study is the necessity to 
observe the clusters at least once every two or three years. When there 



Period Changes of RR Lyrae Variables in Mo bl 

are ten-^"ear gaps l)et\veen series of observations, it l)econies difficult in 
many cases, to know how to draw the diagram. 

From this investigation, it does not appear that the period changes 
are caused by the effects of evolution. However, the time is approach- 
ing when we might expect to be able to determine such changes. 

A ckn oivledgements 

It is a pleasure to acknowledge the help we have received with this 
program. It was supported by a Province of Ontario graduate fellow- 
ship to C. Coutts and b^- grants from National Research Council of 
Canada. We express our gratitude to Dr. H. \V. Bal)cock for the loan 
of the Mount Wilson plates, to Dr. Harlow Shapley and Miss Henrietta 
Swope for consultation about the double exposure plates, to the 
Directors and those staff members of the David Dunlap Observatory 
who have helped with the observational program during the 30 years, 
and to Dr. John Percy for discussion of the phase-shift diagrams. 

Referen'ces 

Arp, H. 1962, Ap. J., 135, 311. 

Bailey, S. I. 1917, Harvard Ann., 78, 157. 

Balazs-Detre, J. and Detre, L. 1965. Remeis-Sternw. Bamberg, Kl. Veroff., 4, no. 40, 

p. 184. 
Barnard, E. E. 1909, .1. N., 184, 273. 

Bartolini, C, Battistini, P. and Nasi, E. 1968, Bologna Pub., 9, no. 15. 
Bartolini, C, Biolchini, R. and Mannino, G. 1965, Bologna Pub., 9, no. 4. 
Belserene, E. P. 1952, .1. /., 57, 237. 

, 1961, .4. J., 66, 38. 

, 1964, A. J., 69, 475. 

Bronkalla, W. 1959, A. N., 285, 181. 

Christy, R. F. 1965, Remeis-Sternw. Bamberg, Kl. Veroff., 4, no. 40, p. 77. 

Dickens, R. J. and Saunders, J. 1965. Royal Obs. Bull, no. 101. 

Faulkner, J. and Iben, I. 1966, Ap. J., 144, 995. 

Fritze, K. 1962, A. N., 287, 79. 

Grubissich, C. 1956, Soc. Astr. Ital. Mem., 27, no. 3. Asiago Contr., no. 76. 

Hett, J. H. 1942, .4. J., 50, 77. 

Izsak, I. 1957, Stern Ungar. Akad. Wiss. Budapest Mitt., no. 42, p. 63. 

Kheylo, E. S. 1964. /. A. U. Inf. Bull. Var. Stars, no. 43. 

, 1965, I.A.U. Inf. Btdl. Var. Stars, no. 104. 

, 1966, I.A.U. Inf. Bidl. Var. Stars, no. 171. 

Kulikov, V. I. 1961, Var. Stars (Russ.), 13, no. 6, p. 400. 

Makarova, V. A. and Akimova, V. P. 1965, Var. Stars (Rtiss.), 15, no. 4, p. 350. 

Mannino, G. 1956a, Soc. Astr. Ital. Mem., 27, no. 3; Asiago Cont., no. 75. 

■ , 1956b, Soc. Astr. Ital. Mem., 27, no. 3; Asiago Cont., no. 76. 

, 1963, Bologna Pub., 8, no. 12. 



58 Christine M. Coiitts and Helen Sawyer Hogg 

Mantegazza, G. P. 1961, Bologna Pub., 8, no. 5. 

Margoni, R. 1964, Soc. Astr. Ital. Mem., 35, no. 2; Asiago Cont. no. 150. 

, 1965a, Asiago Cont., no. 170. 

, 1965b, Remeis-Stermu. Bamberg, Kl. Veroff., 4, no. 40, p. 249. 

, 1967, Asiago Cont. no. 198. 

Martin, W. Chr. 1938, Leiden Ann., 17, pt. 2. 

, 1942, Ap. J., 95, 314. 

Nobili, F. 1957, Soc. Astr. Ital. Mem., 28, no. 2; Asiago Cont., no. 81. 

Xotni, P. and Oleak, H. 1958, A. N., 284, 49. 

Oosterhoft", P. Th. 1941, Leiden Ann., 17, pt. 2. 

Ozsvath, I. 1957, Stern. Ungar. Akad. IViss. Budapest Mitt., no. 42. 

Roberts, M. and Sandage, A. 1955, A. J., 60, 185. 

Sandage, A. 1957, Ap. J., 126, 326. 

, 1965, Comment made at NATO school, Herstmonceux Castle. 

Sawyer, H. B. 1955, David Dunlap Obs. Pub., 2, no. 2. 

Sawyer Hogg, H. and Wehlau, A. 1968, David Dunlap Obs. Pub., 2, no. 19. 

Shapley, H. 1927, Harvard Bull, no. 851, 15. 

Sterne, T. E. 1934a, Harvard Circ, no. 386. 

, 1934b, Harvard Circ, no. 387. 

Szeidl, B. 1965, Stern. Ungar. Akad. Wiss. Budapest Mitt., no. 58. 

Wachmann, A. A. 1965, Uber die Periodenanderungen einiger RR Lyrae-Sterne in 

Kugelhaufen M53. Astronomische Abhandlungen. Professor C. Hoffmeister 

znm 70. Geburtstage gewidmet. Leipzig, J. A. Barth. 
Wilkens, H. 1964, La Plata Sep. Astr., no. 54. 

Richmond Hill, Ontario 
December 30, 1968. 



PUBLICATIONS OF 

THE DAVID DUNLAP OBSERVATORY 

UNIVERSITY OF TORONTO 



Volume 3 Number 2 



STUDIES OF THE VARIABLES IN 
THE GLOBULAR CLUSTER NGC 6171 



CHRISTINE M. COUTTS 

AND 
HELEN SAWYER HOGG 



1971 
TORONTO, CANADA 



PUBLICATIONS OF 

THE DAVID DUNLAP OBSERVATORY 

UNIVERSITY OF TORONTO 



Volume 3 Number 2 



STUDIES OF THE VARIABLES IN 
THE GLOBULAR CLUSTER NGC 6171 



CHRISTINE M. COUTTS 

AND 
HELEN SAWYER HOGG 



1971 
TORONTO, CANADA 



t 



PRINTED AT 
THE UNIVERSITY OF TORONTO PRESS 



STUDIES OF THE VARIABLES IN THE 
GLOBULAR CLUSTER NGC 6171 

By Christine M. Coutts* and Helen Sawyer Hogg 



Abstract 

The purpose of this investigation is to study periods of the variables in NGC 6171 
over a long time interval and to look for period changes in the RR Lyrae stars. The 
study is based on a collection of 47 photographs taken at the David Dunlap Observa- 
tory between 1946 and 1969 and 24 photographs at Cerro Tololo in 1970 combined 
with published observations of other investigators dating back to 1935. 

Twenty-three variable stars have been studied. Twenty- two of these are RR 
Lyrae stars, 10 of which show period changes. One of the variables is a long period 
variable with a period of 332 days. All the variables inside the cluster radius are 
RR Lyraes. 

Introduction 

NGC 6171 (Messier 107, R.A. 16^29'°.7, Dec. -12°57', 1950) is a 
globular cluster with a relatively high metal content. There are 24 
variables which Oosterhoff (1938) discovered on fifteen plates taken 
with the Mt. Wilson 60-inch reflector in 1935. He published magnitudes 
for 23 of the stars and photometer readings for variable 22, which was 
much fainter than the others and below his magnitude sequence. His 
material was not adequate for period determination and the periods 
for these stars were not found until much later. 

Mannino (1961) at Bologna and Kukarkin (1961) at Sternberg both 
investigated the periods of the variables. Mannino's work was based on 
199 photographs taken with the Loiano 60-cm. reflector during 1959 
and 1960. He made visual estimates of the apparent magnitudes for 15 
of the variables and determined periods for 10. Kukarkin took 67 
photographs of the cluster with the 40-cm. reflector at Sternberg, also 
during 1959 and 1960 ; he determined periods for 19 of the stars from 
visual estimates. 

Thirty-one variables beyond the visible boundaries of the cluster 
have been announced. Kurochkin (1962, 1964) found 29, of which 14 
are RR Lyrae and Kukarkin (1962) found 2, for one of which he deter- 
mined an RR Lyrae period. 

*Visiting Astronomer, Cerro Tololo Inter- American Observatory, which is operated 
by the Association of Universities for Research in Astronomy, Inc., under contract 
with the National Science Foundation. 



62 Christine M. CouUs and Helen Sawyer Hogg 

The periods of the variables in the cluster given by Kukarkin and by 
Mannino agree fairly well for all except three, numbers 2, 3, and 8. 
Mannino considered all of these stars to be RR Lyrae variables of 
type c, while Kukarkin's results definitely show them all to be of 
type a, and in all three cases, 

J_ J_ 

where Pk, Pm are the periods by Kukarkin and Mannino respectively. 

Variables 1,11, 20, 22, and 24 were not measured by either Kukarkin 
or Mannino. Variables 1 and 22 were too far from the centre of the 
cluster to appear on their plates, and variables 11, 20, and 24 were too 
close to the centre to be resolved. 

Since we began work on this cluster, Dickens (1970) has published an 
extensive paper on it, making use of some of our unpublished data. He 
studied all the variables except nos. 1, 22, and 24. His work is based on 
25 U, 48 B, and 45 V plates of the cluster, all taken with the Mt. 
Wilson 100-inch telescope in 1966 and 1967. 

Investigations at the David Dunlap Observatory 

The observing program on NGC 6171 was begun by one of us 
(Sawyer Hogg) in 1946 with the 74-inch reflector. The David Dunlap 
Observatory collection includes 46 photographs taken with this tele- 
scope in 10 different years between 1946 and 1969 and one photograph 
(D250) taken with the 16-inch reflector on the campus of the University 
of Toronto in 1969. This material has been supplemented by 24 plates 
taken by Coutts with the Curtis 24-inch Schmidt of the University of 
Michigan on Cerro Tololo in 1970. 

Twenty-three stars have been measured on the David Dunlap plates. 
Variables 6, 7, 8, 9, 11, 20, and 24 were measured visually, the others 
with an iris photometer. Variable 22, probably not a cluster member, 
was again too far from the centre of the cluster to appear on the David 
Dunlap plates and it was not studied. All measures of the variables on 
the Cerro Tololo plates were made with an iris photometer, but vari- 
ables 9, 11, and 24 were too crowded for measurement. The photogra- 
phic magnitudes and heliocentric Julian Days are in Table I. Variable 1 
is considered separately later. All the observations up to and including 
Julian Day 2440393 are from David Dunlap plates; all later observa- 
tions are from Cerro Tololo. 

The adopted periods are listed in Table II, which also gives the 
photographic magnitudes at maximum and minimum light, the ampli- 



TABLE I 
Photographic Magnitudes 



64 



TABLE I. PHOTOGRAPHIC MAGNITUDES 



Dunlap 


Julian Day 


No 


2 


No. 3 


No 


4 


No. 5 


No. 6 


No. 7 


No. 8 


No 


9 


No. 10 


No 


11 


12068 


31970.762 














15.65 


15.95 




16. 


20 




16. 


05 


12116 


76.729 


15. 


67 


15.92 


15. 


91 


15.93 


15.70 


15.95 


15.95 


15. 


80 


16.23 


16. 


05 


12121 


.767 


15. 


84 


16.00 


15. 


63 


15.98 


15.70 


16.05 


16.00 


16. 


00 


16.22 


16. 


05 


12140 


77.709 


16. 


41 


15.54 


15. 


74 


16.17 


15.70 


15.75 


15.40 


15. 


85 


15.41 


15. 


65 


12261 


99.720 














16.10 


16.10 


16,00 


15. 


70 




15. 


85 


12280 


2000.695 














15.85 


16.10 


15.50 


15. 


70 




16. 


25 


12326 


04.682 


15. 


53 


16.09 


15. 


56 


15.66 


16.25 


15.85 


15.55 


16. 


25 


16.32 


16. 


20 


13400 


354.693 


15. 


50 


16.10 






16.03 


16.05 


16.50 


15.95 


15. 


80 


16.06 


15. 


70 


13426 


55.712 


16. 


36 


16.09 


15. 


55 


16.24 


16.00 


16.40 


15.40 


16. 


05 


16.22 


16. 


05 


13446 


56.674 


16. 


28 


15.82 


16. 


06 


15.86 


15.70 


16.45 


16.35 


16. 


00 


15.38 


16. 


00 


13447 


.697 


16. 


30 


15.75 


16. 


09 


15.96 


15.75 


16.40 


16.40 


16. 


30 


15.39 


16. 


00 


13462 


57.675 


15. 


89 


15.62 


15. 


52 


16.19 


16.00 


16.40 


16.35 


16. 


15 


16.23 


15, 


70 


14512 


733.679 


16. 


38 


16.12 


15. 


96 


15.85 


16.30 


16.25 


15.60 


16. 


00 


16.21 


16, 


00 


14517 


.722 


16. 


34 


15.70 


15. 


68 


15.71 


16.00 


16.20 


15.85 


16. 


05 


16.29 


16, 


00 


14536 


34.661 


16. 


22 


16.12 


15. 


77 


16.08 


16.05 


16.15 


16.35 


16. 


10 


16.33 


16 


05 


14542 


.732 


16. 


32 


16.18 


16. 


15 


16.21 


16.20 


16.30 


15.40 


16. 


20 


16.43 


15 


65 


20077 


4538.691 


16. 


34 


15.62 


16. 


04 


16.19 


15.80 


16.25 


16,40 


16. 


00 


16.08 


15 


60 


20229 


72.634 


16. 


02 


15.82 


15. 


85 


15.93 


16.35 


16.50 


16.30 


16. 


00 


16.35 


16 


05 


20241 


73.647 


15. 


91 


16.26 


16. 


05 


16.24 


16.20 


16.20 


15.95 


16. 


05 


16.03 


15 


80 


20275 


75.612 


16. 


23 


15.80 


16. 


11 


16.20 


15.80 


16.30 


16.35 


16, 


10 


15.67 


16 


05 


21416 


930.630 


















16.45 


15, 


70 




15 


95 


21424 


31.636 


















16.35 


15 


75 








22472 


5307.634 


15. 


94 


16.23 


15. 


66 


16.22 


16.25 


16.35 


15.50 


15. 


70 


16,38 


15 


85 


22475 


.673 


16. 


25 


16.28 


15. 


67 


16.25 


16.15 


16,45 


15.65 


15 


65 


16.52 


16 


15 


26830 


8198.715 


16. 


09 


16.01 


15. 


76 


16.26 


15.95 


16.25 


16,40 


16 


15 


15.41 


15 


70 


26833 


.744 


16. 


19 


16.06 


16. 


00 


16.47 


16.10 


15.95 


16.15 


16 


25 


15.66 


15 


70 


26850 


99.679 


15. 


75 


15.53 


16. 


22 


15.86 


15.75 


16.05 










16 


05 


26852 


.702 


15. 


69 


15.84 


15. 


96 


15.80 


15.75 


16.10 


15.90 


16 


10 


16.08 






26856 


.740 


15. 


73 


16.03 


15. 


63 


15.93 


16.00 


16.05 


16.00 


16 


15 


16.36 


16 


10 


27541 


583.724 


16. 


46 


16.24 


15. 


82 


16.09 


16.00 


15.65 


15.54 


16 


10 


16.38 


16 


05 


27545 


84.638 


16. 


14 


15.88 


15. 


88 


16.12 


15.60 


16.00 


16.23 


15 


70 


16.36 


15 


60 


27561 


87.712 


16. 


18 


15.96 


15. 


70 


16.30 


15.60 


15.60 


15.73 


15 


90 


15.72 


15 


70 


29101 


9265.794 


16. 


00 


16.33 


16, 


13 


15.95 


16.10 


16.25 


15.95 


15 


60 


16.20 


15 


95 


29105 


.837 


16, 


05 


16.45 


16, 


18 


15.39 


16.25 


16.25 


16.10 


15 


60 


15.27 


16 


10 


29144 


70.834 


15, 


70 


16.32 


15. 


81 


15.58 


15.85 


16.25 


15.85 






15.41 


16 


10 


29160 


71.738 






15.75 


16. 


16 


16.12 


15.85 


15.80 


16.15 


16 


05 


15.78 


16 


05 


29166 


39271.787 


16 


40 


15.97 


15 


91 


16.14 


15.95 


16,10 


15.45 


16 


05 


15.87 


16 


15 


29171 


.834 


16 


25 


15.98 


15 


87 


16.05 


16.15 


16.05 


15.20 


15 


95 


16.20 


16 


25 


29557 


357,580 






16.13 


15 


77 


16.35 


15.65 


15.60 


15,90 


15 


65 


16,20 


15 


80 


32128 


40354.772 


15 


75 


16.02 


16 


05 


16.10 


16.05 


16.10 


15.65 


16 


20 


16.10 






32142 


56.807 


16 


50 


15.61 


16 


02 


16.00 


16.10 


16.00 


16.15 


15 


85 


16.20 






D250 


82.735 


16 


05 


16.06 






15.92 


15.70 


15.60 


15.35 






16.22 






32203 


89.690 


16 


05 


15.80 


15 


70 


15.95 


15.75 


15.70 


16.15 


16 


10 


16.10 


15 


80 


32206 


.733 


16 


30 


16.10 


15 


98 


16.05 


15.60 


15.60 


16.40 


16 


05 


16.31 


16 


05 


32210 


.777 


16 


15 


16.11 


16 


05 


16.10 


15.75 


15.85 


16.25 


15 


95 


16.20 


16 


05 


32228 


93.703 


16 


25 


15.95 


15 


95 


16.40 


15.90 


15.55 


16.25 


15 


60 


15.65 






32231 


.745 




















15 


55 


15.95 






C.T.I. 


O 






























6408 


691.892 


16 


54 


16.34 


16 


00 


16.15 


16.18 


15.94 


15,50 






15.70 






6417 


92.681 


16 


15 


15.92 


15 


96 


16.23 


15.71 


15.88 


16,06 






15.86 






6428 


,889 


16 


06 


16.21 


16 


12 


16.27 


15.92 


15.96 


15.04 






15.16 






6438 


93.681 


16 


72 


15.98 


16 


18 


16.25 


15.67 


15.90 


15.86 






15.25 






6443 


.801 


16 


53 


16.10 


15 


84 


16.06 


16.00 


15.90 


15.98 






15.82 






6447 


.874 


15 


88 


15.98 


15 


83 


16.13 


16.43 


16.03 


15.85 






15.93 






6477 


94,912 


16 


69 


15.88 


15 


88 


16.40 


16.24 


15.90 


16.09 






15.20 






6491 


95.878 


16 


42 


16.27 


16 


21 


16.11 


15.63 


15.86 


15.59 






15.67 






6650 


708.793 


16 


01 


16.23 


15 


84 


16.17 


16.00 


16.07 


15.92 






15.84 






6927 


45.631 


16 


53 


16.35 


16 


23 


16.20 


16.32 


15.98 


15.55 






15.06 






6931 


47.669 


16 


18 


16.19 


16 


02 


16.35 


16.16 


15.92 


15.92 






15.03 






6945 


49.679 


16 


46 


16.27 


15 


72 


16.27 


15.76 


16.29 


16.00 






15.83 






7031 


801.476 


16 


45 


16.00 


16 


41 


16.23 


15.98 


15.47 


15.69 






15.47 






7043 


.606 


16 


64 


16.39 


15 


90 


16.43 


16.16 


15.88 


15.61 






15.54 






7065 


02.586 


16 


35 


16.04 


16 


19 


16.00 


16.17 


15.80 


15.61 






15,18 






7077 


03.486 


16 


00 


16.39 


16 


22 


16.20 


16.30 


15.45 


15.88 






15.37 






7087 


.632 


16 


20 


15.90 


15 


94 


16.16 


16.06 


15.96 


15.73 






15.59 






7107 


05.663 


16 


47 


16.17 


16 


21 


16.25 


15.81 


16.09 


15.72 






16.00 






7115 


06.493 


16 


21 


15.98 


16 


12 


16.41 


16.10 


15.59 


16.15 






15.82 






7119 


.560 


16 


19 


16.04 


16 


35 


16.41 


16.19 


15.92 


15,37 






15.81 






7145 


08.469 


16 


68 


16.17 


16 


43 


16.37 


15.53 


15.52 


15,94 






15.80 






7155 


.613 


15 


86 


16.20 


15 


73 


16.17 


16.00 


15.84 


15,81 






15.86 






7166 


09.536 


16 


35 


16.29 


15 


84 


16.19 


15.65 




15,65 






16.10 






7172 


.634 


16 


54 


16.15 


16 


23 


15.92 


15.78 


15.96 


15,59 






15.24 







No. 13 No, 14 No,15 No, 16 No.l7 No, 18 No. 19 No. 20 No. 21 No.23 No. 24 



65 









16,10 












15,75 






15 


25 


16.18 


16 


.43 


16,20 


15.63 


16.43 


16.29 


15,75 


15.92 


15.75 


16,29 


16.05 


15 


85 


16.23 


16 


.43 


16,30 


15,80 


16.38 


16.31 


15,74 


15.88 


15,65 


16.28 


16,14 


15 


75 


16.40 


16 


.52 


16.20 
16,10 
16,15 


16,12 


16.26 


16,17 


16,31 


16.12 


15,45 
16,00 
15,30 


16,65 


16,08 


15 
15 
15 


95 
95 
90 


16.40 


16 


.20 


16,15 


15,71 


15.60 


16,16 


16,38 


15,89 


15.35 


16,53 


15,90 


15 


20 


16.54 


15 


,67 


16.15 


16,03 


16.26 


15,87 


16,53 


16.10 


15.60 


16,38 


15,88 


15 


45 


16.44 


16 


,20 


16.60 


16,10 


16.52 


15,44 


16.38 


16.28 


15.55 


16.55 


16,04 


15 


35 


16.48 


16 


30 


16.35 


16.19 


15,97 


16,45 


16,00 


15.81 


16.00 


16,56 


16.23 


15 


95 


16.55 


16 


.52 


16.20 


16,21 


16,12 


16,37 


16.10 


15,76 


15,80 


16.49 


16,24 


16 


05 


16.58 


16 


56 


16.40 


15,60 


15,82 


16.21 


15.79 


16.25 


15,80 


16,79 


16,17 


15 


85 




15 


30 


16. 15 


15,69 


16,12 


16.28 


16.07 


16.12 


15,55 


16,56 


16,08 


16 


05 


16.45 


15 


75 


16.15 


15,82 


16,25 


16.26 


16.27 


16,36 


15.40 


16,78 


16,22 


16 


00 


16.67 


15 


60 


16.05 


16.09 


15,89 


16,12 


16.01 


15,88 


15.85 


16,41 


16.11 


15 


80 


15.25 


16 


32 


16.35 


16.29 


16.13 


16,24 


15.77 


15.92 


15,95 


16,65 


16.28 


15 


85 


15.66 


16 


57 


15.65 


16,27 


16,35 


15,88 


16.38 


16.18 


15.65 


16,38 


16.19 


15 


80 


16.41 


16 


58 


16.15 


15,93 


16.29 


16.30 


16,53 


16,01 


15,45 


16,78 


16.18 


15 


65 


15.46 


16 


50 


16.15 


16.16 


16.33 


16.23 


16.36 


16,20 


15,70 


16,68 


16.13 


15 


45 


15.80 


16 


72 


16.60 
15.45 
15.50 


16.19 


15,88 


15.40 


16.51 


15,90 


15,50 
15.55 


16,44 


15.83 


16 
15 


05 
95 


16,30 


15 


79 


16.45 


15.85 


15,88 


16.26 


16,57 


16,15 


15.65 


16,49 


16.02 


15 


20 


15.65 


15 


98 


16.50 


15,89 


15,96 


16.38 


16,07 


15,96 


15,75 


16,46 


15.90 


15 


30 


16.09 


16 


45 


16.25 


15,83 


16,00 


16,12 


16,39 


16,03 


15,60 


16,38 


15,78 


15 


85 


16.40 






16.20 
16.50 


15.83 


15.95 


16,28 


16,44 


15.82 


15,65 


16,37 


15.70 


15 
15 


70 
55 


16.37 


16 


56 


16,20 


16,17 


15.78 


15.88 


16,05 


16,38 


15,45 


16,68 


15.65 


16 


00 


16.44 


16 


55 


16.15 


16,17 


15.90 


16,05 


16.30 


16,28 


15,25 


16,59 


15.84 


16. 


15 


16.44 


16 


33 


15,60 


15,98 


16,48 


16.44 


16,40 


15,97 


15,85 


16.66 


16.39 


15. 


95 


16.43 


16 


14 


15,40 


16.19 


16,22 


16.03 


16,30 


16,14 


15.90 


16.36 


16.35 


15. 


70 


15.76 


16 


26 


16,20 


15,66 


16,07 


16,16 


16,37 


16,26 


15,40 


16,33 


15.86 


15. 


65 


16.01 


16 


15 


15,65 


16,17 


15,97 


15,49 


16,08 


15,83 


15,55 


16,35 


16.04 


15. 


55 


15.70 


16 


40 


16,00 


15,99 


16,17 


15,75 


16,05 


15.49 


15.55 


16.45 


16.11 


15. 


70 


16.15 


15 


85 


16,15 


15,62 


16,42 


15,45 


15,75 


15,74 


15.70 


16,55 


16.15 


15. 


95 


16.05 


15 


95 


16,10 


15.90 


16,40 


16,24 


16,48 


15.94 


15,85 


16,30 


16.20 


15. 


55 


16.30 


16. 


23 


16.15 


16,15 


16.46 


16,28 


16,45 


16.38 


15.85 


16,50 


16.30 


16. 


15 


16.25 


16, 


41 


16,15 


16.11 


16.53 


16.53 


16,31 


16.39 


15.75 


16,55 


15.95 


16. 


00 


15.88 


15. 


62 


16.15 


16.15 


16.50 


16.31 


16.16 


15.80 


15.70 


16,55 


16.05 


15. 


70 


16.05 


16. 


10 


16.00 


15.71 


15.96 


16.14 


16.51 


16.15 


15.70 


16.50 


15,95 


16, 


10 








16.15 


15.89 


16.43 


16.02 


16,54 


16.10 


15,75 


16,65 


15,93 


15, 


70 


16.40 


16. 


05 


16.10 


15.82 


16,08 


16,17 


16,34 


16.54 


15,55 


16,35 


16,28 


15, 


30 


16.12 


15. 


89 


16.25 


15.89 


16,59 


16,19 


16,68 


16.00 


15.45 


16,30 


15,85 


15. 


90 


16.23 


16. 


16 


15.55 


15.95 


16.70 


16.05 


16.26 


16.19 


15.65 


16,45 


16,00 


16. 


10 


16.34 


16. 


37 


15.20 


16,07 


16.21 


15.43 


16.32 


16,08 


15.70 




15,99 


16, 


10 


16.05 


16. 


50 


15.55 


15,82 


16.24 


15.30 


16.30 


15,70 


15,45 


16,60 


16,03 


15, 


65 


16.07 












15.44 










16.23 






15.66 


16. 


13 


16,22 


15,95 


16.36 


15.79 


16,02 


16,39 


15,15 


16,46 


16.30 






15,69 


15. 


88 


15.24 


15.86 


15.90 


16.18 


16,46 


16,35 


15.38 


16.51 


16,12 






15.68 


16. 


25 


16.22 


16,03 


16.37 


15.52 


16,56 


16.07 


15.30 


16,60 


16,12 






15.60 


16, 


10 


15.32 


16,17 


16.01 


16,09 


16,28 


16.17 


15,10 


16,48 


15,90 






15.60 


16. 


46 


16.20 


16,10 


16,30 


16,24 


16.39 


16,50 


15,15 


16,47 


16.33 






15.90 


16, 


34 


16.32 


15.85 


16,13 


15,93 


16,40 


16.18 


15,34 


16,63 


16,18 






16. 13 


15, 


28 


16,40 


16,27 


16,38 


16.26 


16,60 


16,46 


15,20 


16.80 


16,03 






15.97 


15. 


49 


16,30 


15,84 


16,27 


16.11 


15,97 


16,03 


15,38 


16.46 


16.11 






15.70 


16, 


30 


16,15 


16,23 


15,76 


16,05 


16,13 


16.19 


15,20 


16.36 


16.14 






15.71 


16. 


23 


16.32 


16,25 


16,39 


15,59 


16.31 


16.37 


15,18 


16,53 


16.23 






15.41 


15. 


45 


15,69 


16,20 


16,33 


16,20 


16,60 


16.39 


15.24 


16.60 


16.02 






15.86 


16, 


08 


16.14 


16,25 


16,16 


15,96 


16,31 


15,96 


15,18 


16.70 


16.14 






15.44 


15, 


96 


16,23 


15,88 


16,25 


16,08 


16,02 


16,20 


15,20 


16,35 


16,35 






15.59 


16, 


23 


15,67 


16,04 


16,31 


16,12 


16,56 


16,27 


15,40 


16.70 


16.06 






15.65 


16, 


26 


15,71 


16,10 


16,22 


15,96 


16,12 


16,37 


15,13 


16,44 


16.12 






15.54 


16, 


25 


15.24 


15.88 


16,10 


15,71 


16,70 


16,08 


14,94 


16.52 


16.37 








16. 


15 


15,86 


16.12 


16,29 


15.88 


15,84 


16.45 


15.14 


16,49 


15.92 






15.82 


16. 


00 


16,15 


16.17 


16.27 


15,55 


16.58 


16,20 


15.22 


16,43 


16.19 






16.08 


15. 


45 


16.16 


16,08 


16,17 


16.15 


15,92 


16,33 


15.06 


16.74 


15.92 






15.94 


15, 


86 


16.29 


16,16 


15.79 


16.22 


16, 17 


16,00 


15.26 


16.76 


15.94 






16.20 


16. 


35 


15.96 


15,94 


16.58 


15.76 


16,62 


16.09 


15.32 


16.35 


16.10 






15.42 


16, 


18 


16.17 


16.06 


15.90 


15.94 


16,80 


16.27 


15,28 


16.80 


16,14 






(5.49 


15. 


98 


16,15 


16.00 


16.51 


15.45 


16,45 


16.29 


15,13 


16.31 


16.32 






15.84 


16, 


12 


16,02 


15.74 


16.29 


15.88 


16,37 


16,00 


15.12 


16,88 


16.22 







66 



Christine M. Coutts and Helen Sawyer Hogg 



TABLE II 
Elements of Twenty-three Variables 





Photograph 


c 












Magnitude 




















Epoch 


Period 


& 














Variable 


Max. 


Min. 


Amp. 


of Max 


days 


days/10«yr. 




1 


14.0 


17.0 


3.0 


40504. 


332. 






2 


15.6 


16.4 


0.8 


40389.502 


0.5710205 






3 


15.55 


16.25 


0.7 


40389 . 595 


0.566343 






4 


15.5 


16.15 


0.65 


40389.628 


0.2821317 






5 


15.7 


16.25 


0.55 


40389.709 


0.70238 


0.9 




6 


15.7 


16.25 


0.55 


40389.740 


0.2602558 






7 


15.6 


16.55 


0.95 


40389.696 


0.49959 


-0.15 




8 


15.4 


16.45 


1.05 


40389.957 


0.559921 


-0.25 




9 


15.95 


16.35 


0.4 


40389.583 


0.3206025 


0.15? 




10 


15.4 


16.6 


1.2 


40389.532 


0.4155329 


1.1 




11 


15.8 


16.45 


0.65 


40389.611 


0.592808 


-0.21 




12 


15.25 


16.5 


1.25 


40389 . 593 


0.472956 


2.2to -1 


1 


13 


15.35 


16.6 


1.25 


40389.596 


0.466797 






14 


15.4 


16.5 


1.1 


40389 . 763 


0.4816129 


0.5 




15 


15.6 


16.25 


0.65 


40389.687 


0.2885895 






16 


15.65 


16.5 


0.85 


40389.853 


0.5228709 


-1.6 




17 


15.4 


16.45 


1.05 


40389.761 


0.561154 






18 


15.75 


16.5 


0.75 


40389.898 


0.564378 






19 


15.75 


16.3 


0.55 


40389.822? 


0.2787622 






20 


15.65 


16.4 


0.75 


40389.653 


0.5781113 






21 


16.3 


16.6 


0.3 


40389.704 


0.258125 






23 


15.5 


16.2 


0.6 


40389.725 


0.3233436 






24 


15.65 


16.45 


0.8 


40389.615 


0.3462153 


-0.35? 





Remarks to Table II 
Variables for which no/3 is given here are considered as having constant periods and 
their light curves are shown in Figure II. Values of ^ have been determined on the 
assumption of linear period change, as represented in the phase shift diagrams in 
Figure I. 



V7 



V9 
Vll 



V12 



V20 
V21 
V24 



Period derived from Kukarkin's alternate period 0.4996. His favoured period 
0.3332065 did not fit the David Dunlap observations. Period decrease seems 
indicated but a constant period is not ruled out. 

Period increase seems indicated, but a constant period is not ruled out. 
Adopted period derived from that of Dickens (0.59280). The value of /S is 
uncertain. The phase-shift diagram is better represented by an abrupt change 
of period than by a linear change (i.e. two intersecting straight lines rather than 
a parabola). 

The assumed period indicates both an increase and decrease of period over the 
35 year interval. If instead, the phase-shift diagram was constructed with 
P = 0.472972, a period decrease of 1.6 days per million years would be indi- 
cated. The adopted period is that which gives the smaller dispersion of points 
in the phase-shift diagram over the 35 year interval. 
Period derived by us and confirmed by Dickens. 
Probably not a cluster member. 

Period derived by us, but uncertain because there were no observations by 
Kukarkin, Mannino or Dickens. An alternate period, P = 0.529586 is possible. 



Studies of the Variables in the Globular Cluster NGC 6171 67 



02 


— 1 r 

.2 


1 T T 


-I r 

7 


1 1 1 


00 


♦ 


♦ + f ♦♦^ - 


■ ♦ 


^ S^i^ - 




■ 


* 






02 


. 3 




8 


- 


00 


- k 


♦ ♦ + ^♦s . 


■ ♦ 


♦ ♦ ++M^ : 




4 




9 


. 


oo 


- \ 


1 1 


1 1 


" 1 H^f ■ 


•0 2 


- 








5 




10 




0-2 








■ 





- + 


• ...it " 


( 1 




02 


- 






( 1 


•04 


■ 










6 




II 




0-2 








1 


00 


- ♦ 

1 i 


• ' ( t^• ■ 

1 1 1 - 


■ 1 

1 1 


L 1 1 



1930 40 50 60 70 1930 40 50 60 70 



Fig. 1 — Phase-shift diagrams (phase-shift vs. year). The marks along the vertical 
axis are one tenth of a cycle apart. Vertical bars represent probable errors. 



68 



Christine M. Coutts and Helen Sawyer Hogg 





J2 


— 1 1 1 


18 


T 1 1 


00 


- 1 


+ Nf+ - 


■ \ 


\ \ ^\>»^ - 


-02 




1 




- 




13 




19 




CO 


- \ i 


. • t 4*1 ■ 


• + 


f ^*^*^ : 




14 




20 




GO 


— 1 


1 




■ k 


1 4 H^^ : 


-0 2 


. 




■ 




15 




21 




00 


- k { 


^ *^|#* • 


1 1 


i f M^»4 - 




' 




- 




16 




23 




2 


^ 


^ M 




. 


00 


- f 


\ - 


• \ 


♦ M^^ - 


04 


. 17 




24 


- 


2 


- 






( 


' i - 


00 


- 4 \ 


, ,,M . 


1 1 


1 


( • _ 

1 




■ 






- 


-02 


1 1 


1 1 1 


1 1 


1 1 


• 



1930 40 50 60 70 B30 40 50 60 70 

Fig. 1, cont'd — Phase-shift diagrams (phase-shift vs. year). The marks along the 
vertical axis are one tenth of a cycle apart. Vertical bars represent probable errors. 



Studies of the Variables in the Globular Cluster NGC 6171 



69 



tudes, the epochs of maximum light and /3, the rate of period change in 
days per milHon years. The periods were derived from those of Kukar- 
kin (1961) except for variable 7, where we chose his alternate period, 
and variables 1,11, 20, and 24. Dickens (1970) has studied variables 11 
and 20 ; he confirmed a value of the period for variable 20 which we 
communicated to him (Coutts 1964), but ruled out our period for 
variable 11 so the period we have adopted for this star is based on his 
value. We are not certain about our value for the period of variable 24 
and have suggested an alternative, but it does not lit the observations 
as well. 



150 



15-5 



160 



15-5 



160 



16-5 



15-5 



160 



16-5 



V20 






1 

P=0 578III3 



••••• t»« 

• • • • . • 



V3 



P=0 566343 



r. 



'^tr .^^i. 



VI7 



P=0-56II54 






• V 



tfi o 



V2 



,a • 



1 

P=057I0205 



^o 



a1^^ 



.A. 8*. 






VIS 



P=0-564378 






^' 



0° 



^V 



>^.>, 



^fi 



VI3 



P=0-466797 






^4° • °^ 









A« 



16-0 



160 



160 



Fig. 2 — Light curves for stars with constant periods. The phase is in fractions of a 
period. Triangles represent the observations from Mt. Wilson (1935), closed circles 
from the David Dunlap Observatory, and open circles from Cerro Tololo. For 
variable 20, only the David Dunlap observations are plotted because there are large 
systematic differences in magnitudes between the observations from different 
observatories. 



70 



Christine M. Coutts and Helen Sawyer Hogg 



155 
160 
16 5 


1 1 1 
' V 23 ^ P = 0-3233436 " 

\^*^:* °°o;.A ^ • 


1 1 1 

" '^ '^ /^^i«A P=0 2885895" 

o# '^•V A 

• ,o° oo«,? 


15-5 
160 
I6-5 


. V4 P0282I3I7 . 

o o T» o o o S*y 
o 
o o o 


. V 19 • P--0-2787622 . 

t '*^.A.^ 

*• ;fe " ° ^-^ .A- ; 

• o o % * A^ , o 
'& ftctom O e 


15-5 
160 
165 


^ V6 •• • P= 2602558 ' 

• A*^ ^» ^ 

- •- • • • 4"— * •• ■ 

1 1 1 


" V 21 P=0-2583I25 " 

O o 



160 



- 16 



160 



Fig. 2, cont'd — Light curves for stars with constant periods. Triangles represent 
the observations from Mt. Wilson (1935), closed circles from the David Dunlap 
Observatory, and open circles from Cerro Tololo. For variable 6, only the Mt. 
Wilson and David Dunlap observations are plotted because the star is not resolved on 
the Cerro Tololo plates and the magnitudes are brighter. 



We have investigated the variables for period changes by the method 
described by Belserene (1964). Using the periods of Table II, light 
curves for the Mt. Wilson 1935 observations were drawn on tracing 
paper and fitted to the curves for other years to determine the phase 
shifts. The phase shift data are shown in Table III and the diagrams in 
figure 1. For twelve of the stars, no period change is indicated over the 
time interval 1935-1970. Light curves for these stars are shown in 
figure 2. For the stars which have period changes, /3 has been calculated 
as for Messier 5 by Coutts and Sawyer Hogg (1969). Standard parabo- 
las for different values of /3/P^ were fitted visually to the phase shift 
diagrams and the best value of ^ calculated. These values of are listed 
in Table II and the relationship between ^ and period is shown in 
figure 3. 



Studies of the Variables in the Globular Cluster NGC 6171 



71 



u 


o 
rt 


J 


u 


< 


_C 


H 


tn 




H 




U. 








K 




CAl 




W 




(/I 




< 




K 




(X 



I I I 



OO 0> GOOJ iM 
OO O ^ OO 



MM 



M I M M 



ooooooooo 



M M M M 



I M M M 



•^ lO CO to CD 
I I I I I 

lOCOCOOlCOcOcOOlO 
CO-^iOiOCOCOCDCOt-- 



o 




o 


ooo ooooo 


O 


M 1 M 1 


o> 


ooooooo o 


o 


1 1 1 



I I 



O^coiOiooiMroio 
ooooooooo 



I I I 



MM 



00 lo o Tt< r^ 

^ lO CO CO CO 

I I I I I _ 

iCCOCOCncOCDcOOiO 

co-^ioiococococoi~- 



72 



Christine M. Coutts and Helen Sawyer Hogg 



^ 



1-2 


1 


1 


1 1 1 


- 


0-8 


_ 


« 


_ 




- 




( 


- 


04 


- 




- 


C\C\ 


~ 1 


1 




- 


\>\j 






V 


» 

(1 n 


- 


-0-4 


- 


( \ 




1 


- 


-as 


- 






- 


-1-2 


- 




• 




- 


-1-6 


- 




1 1 


- 


-20 


1 


1 


1 


1 1 


- 



0^ 



0-4 



0-5 



0-6 



07 



Fig. 3 — The rate of change of period /3 (in days per million years) vs. period (in 
days). Vertical bars represent the probable errors in /3 for stars with changing periods. 



Variable 1 

Variable 1 (V720 Oph) is a long period variable. It is located 8'. 9 
from the centre of the cluster. The cluster radius is given as 6'.4 by 
Kron and Mayall (1960). Owing to the distance of this variable from 
the centre of our plates and the fact that it is brighter than the standard 
sequence of Oosterhofif at maximum and fainter at minimum it is 
difficult to determine the magnitudes accurately. In Table IV, we give 
mean photographic magnitudes and mean Julian Days for all observa- 
tions separated by less than a week. The period of this variable appears 
to be very long, 332 days. Its light curve is shown in figure 4. According 
to Feast (1965), no Mira variables with periods greater than 220 days 
have been found to be members of globular clusters. He is currently 
working on the important problem of the membership of this star. 



Studies of the Variables in the Globular Cluster NGC 6171 73 



14 - 



15 - 



16 



17 



MA. »A A 



MA •A A 



0-5 0-5 

Pig. 4 — Light curve for variable 1. The phase is in fractions of a period. Open 
circles represent the observations of 1935, closed circles 1946-48, open triangles 
1953-55 and closed triangles 1963-70. 

TABLE IV 
Mean Points for Light Curve of Variable 1 



Julian Day 



Magnitude 



31970 
32000 
32328 
32355 
32734 
34540 
34570 
34930 
35308 
38199 
38585 
39265 
39357 
40355 
40390 
40449 
40692 
40708 
40747 
40801 
40809 
40862 
40870 
40880 



14.85 

15.75 

15.5 

16.15 

17.0 

14.1 

14.1 

15.5 

15.9 

14.2 

15.25 

16.0 

17.0 

17.0 

17.0 

14.0 

17.0 

17.0 

14.7 

14.0 

14.0 

14.0 

14.0 

15.0 



74 Christine M. Coutts and Helen Sawyer Hogg 

Discussion 

There are twenty-two RR Lyrae variables in NGC 6171. Of these, 
fourteen are of Bailey type a, b and eight type c. One of the type c 
variables, no. 21, is fainter than the others and is probably not a cluster 
member. Dickens (1970) excludes this variable from his discussion of 
the properties of RR Lyrae variables in NGC 6171. The number of 
RR Lyrae type c variables is therefore seven. The mean period of the 
a, b stars is 0.54 days, and of the type c stars 0.29 days. These periods 
are short for their types, a feature which is characteristic of relatively 
high metal content. This is expected because the Morgan class of the 
spectrum is V (Sandage and Katem 1964) and in the colour-magnitude 
diagram, the horizontal branch is heavily populated on the red side of 
the RR Lyrae gap (van Agt 1961, Sandage and Katem 1964). The 
period-amplitude relation is shown in figure 5 and the period-frequency 
distribution in figure 6. These diagrams indicate that NGC 6171 is a 
cluster of the Oosterhoff type I, or, as Dickens (1970) notes, it might 
even represent a somewhat shorter period group. 

We have found that almost half of the variables show period changes 
during the 35 year interval of observations. Four have increasing 
periods (median rate 0.7 days per million years) and five decreasing 
(median rate 0.25 days per million years). One variable, no. 12 appears 
to have had an increase and a decrease in its period over the 35 year 
interval. Behaviour like this raises doubt that observed changes are 
caused by evolutionary effects in the stars. Also it can be seen from 
figure 1 that the observations for both variables 10 and 11 would be 
better represented by two intersecting straight lines (indicating an 
abrupt period change) than by a parabola (indicating a uniform 
change). This problem of the interpretation for phase-shift diagrams 
was discussed for six stars in M5 by Coutts (1969) who concluded that 
the hypothesis of abrupt period change was usually better than that of 
the uniform change. 

The period changes for these variables in NGC 6171 are large com- 
pared with those in M5 where 20 stars have increasing periods (median 
0.05 days per million years) and 12 have decreasing periods (0.075 days 
per million years). However, we must keep in mind the fact that with 
observations over a time interval of only 35 years in NGC 6171, the 
minimum value of /3 that can be detected when P = 0.5 is 0.15 days 
per million years. 

The period changes of the RR Lyrae variables in M3 are of about the 
same order of magnitude as those we observe in NGC 6171 and in both 
clusters there are about the same number increasing as decreasing. On 
the other hand, almost all the RR Lyrae stars investigated in w 



Studies of the Variables in the Globular Cluster NGC 6171 75 



*pg 





- 


1 






1 


1 
• • 




1 


1 


- 


1-2 


- 








• 


• 




• 




- 


10 


- 










• 


• 






- 


0-8 


- 


•• 




• 








• 

• • 
• 
• 




- 


0-6 


" 


• • 


• 












• 


; 


0-4 


- 


• 

1 


• 




1 


1 




1 


1 


- 



0-3 



0-4 



0-7 



0-5 0-6 

P 

Fig. 5 — Period-amplitude relation. The amplitude in photographic magnitudes 
was calculated from the David Dunlap observations. 



6 - 

N - 

4- 



2' 






0-2 



0-4 



0-6 



Fig. 6 — Period-frequency distribution of the RR Lyrae stars. 



Centauri show increases in period. If the observed dispersion in period 
changes is due to some random noise as Iben and Rood (1970) com- 
mented, it would appear that the RR Lyrae periods are increasing at a 
rate of 0.1 days per milHon years. These authors pointed out that one 
of their models for horizontal branch stars (Y = .30, Z = 10~*) gave a 
reasonable fit to the observed period changes of the RR Lyrae stars in 
CO Centauri. They found that a model with Y = 0.30, Z = 10~^ gave an 
approximate fit to the observations in M3. It appears that the period 
changes found for the variables in AI5 and NGC 6171 are similar to 
those in M3 and give a reasonable fit for Iben and Rood's models. 
However, if the observed increases and decreases are both caused by 
evolutionary effects, most theories indicate that increases and decreases 



76 



Christine M. Coutts and Helen Sawyer Hogg 



154 - 



<V> - 



15-6- 




15-8- 



<B-V> 

Fig. 7 — Colour-magnitude plot of the RR Lyrae variables in NGC 6171. The data 
are taken from Dickens (1970). Arrows pointing to the right indicate period increases; 
and those to the left, period decreases. 



should be at different rates and consequently we should find more 
periods changing in the direction in which the evolution is slower. This 
is not the case in any of these clusters. 

Figure 7 shows the positions of the RR Lyrae variables in a colour- 
magnitude plot. The data have been taken from Dickens (1970). 
Arrows indicate the direction of the period change (if any). The most 
noticeable feature of this diagram is the absence of period change 
among the type c variables with (B — V ) <0.60. It is possible that 
these stars have constant periods because they are changing the direc- 
tion of their evolutionary path in the HR diagram. 

At the present time, it seems doubtful that the observed period 
changes are caused by evolution of the stars. It is interesting to note, 
however, that the period changes indicate a difference between u 
Centauri and ]M3, M5 and NGC 6171. These latter clusters are of the 
Oosterhoff type I while w Centauri belongs to the longer period type II 
group. Belserene (1956) pointed out that w Centauri appears to be a 
cluster relatively poor in RR Lyrae variables when their numbers are 
compared with all the other horizontal branch stars. On the other hand, 



Studies of the Variables in the Globular Cluster NGC 6171 11 

according to her investigation MS and M5 are richer and NGC 6171 is 
one of the richest clusters. The reality of the separation of the clusters 
into two groups according to the period changes of their RR Lyrae 
stars can be better established when the variable rich and metal poor 
cluster M15 is reinvestigated. 

A cknowledgements 

It is a pleasure to acknowledge the help we have received with this 
program. It was supported by a Province of Ontario Graduate Fellow- 
ship to C. M. Coutts and by grants from the National Research Coun- 
cil of Canada. We express our gratitude to the Directors and staff of 
the David Dunlap Observatory who helped with the observational 
program during the 24 years and also to Dr. Victor Blanco and the staff 
of the Cerro Tololo Inter-American Observatory for making observing 
time on the Michigan Schmidt telescope available to us. 

References 

van Agt, S. L. Th. J. 1961, B.A.N., 15, 327. 

Belserene, E. P. 1956, Contrih. Rutherford Ohs. No. 33, 13. 

, 1964, A. J., 69, 47.5. 

Coutts, C. M. 1964, Master's Thesis, University of Toronto. 

Coutts, C. M. and Sawyer Hogg, H. 1969, David Dunlap Obs. Publ., 3, no. 1. 

Dickens, R. J. 1970, Ap. J. Supplement, no. 187. 

Feast, M. \V. 1965, Obs., 85, 16. 

Iben, I. and Rood, R. T. 1970, Ap. J., 161, 587. 

Kron, G. E. and Mayall, N. U. 1960, A. J., 65, 581. 

Kukarkin, B. V. 1961, Peremennye Zvezdy Bjull., 13, 384. 

, 1962, Peremennye Zvezdy Bjull, 14, 21. 

Kurochkin, N. E. 1962, Peremennye Zvezdy Bjull., 14, 15. 

, 1964, Peremennye Zvezdy Bjull., 15, 164. 

Mannino, G. 1961, Bologna Pub., 7, no. 18. 

Oosterhoff, P. Th. 1938, B.A.N. , 8, 273. 

Sandage, A. and Katem, B. 1964, Ap. J., 139, 1088. 

SzeidI, B. 1965, Stern. Ungar. Akad. Wiss. Budapest Mitt., no. 58. 

Richmond Hill, Ontario 
May 26, 1971 



I 



PUBLICATIONS OF 

THE DAVID DUNLAP OBSERVATORY 

UNIVERSITY OF TORONTO 

Volume 3 Number 3 



VARIABLES IN MESSIER 5: 

A STUDY OF MOUNT WILSON 

1917 OBSERVATIONS 



CHRISTINE M. COUTTS 



1971 
TORONTO, CANADA 



PUBLICATIONS OF 

THE DAVID DUNLAP OBSERVATORY 

UNIVERSITY OF TORONTO 

Volume 3 Number 3 



VARIABLES IN MESSIER 5: 

A STUDY OF MOUNT WILSON 

1917 OBSERVATIONS 



CHRISTINE M. COUTTS 



1971 
TORONTO, CANADA 



PRINTED AT 
THE UNIVERSITY OF TORONTO PRESS 



VARIABLES IN MESSIER 5: 
A STUDY OF MOUNT WILSON 1917 OBSERVATIONS 

By Christine M. Coutts 



Abstract 

This paper portrays the light curves and gives the epochs of maximum light for 
62 variables from Shapley's 1917 collection of photographs of M5. This completes 
the publication of their magnitudes. 

Messier 5 is the fifth globular cluster in richness of variable stars, 
being surpassed only by Messier 3, Omega Centauri, IC 4499 and 
Messier 15. Of its 97 variables, 93 are of the RR Lyrae type. The other 
types represented are W Virginis (nos. 42 and 84), irregular (no. 50) 
and SS Cygni (no. 101). Periods have been determined for 91 of the 
RR Lyrae stars (Bailey 1917, Shapley 1927 and Oosterhoff 1941). 
Period changes have been investigated by Coutts and Sawyer Hogg 
(1969), and independently by Kukarkin and Kukarkina (1969). 

This paper presents the results from the measurement of Shapley's 
collection of photographs taken with the Mount Wilson 60-inch tele- 
scope on eight difTerent nights in 1917. When the periods were 
published by Shapley in 1927, the individual magnitudes from the 
plates were not given. For the above-mentioned study of the period 
changes. Dr. H. W. Babcock, Director of the Hale Observatories, 
kindly lent us the plates for measurement. The 1917 series on Seed 27 
blue-sensitive emulsion consists of 115 exposures on 59 plates. Most of 
the plates have double exposures with the two images separated by 
approximately half a millimetre. Previously (Coutts and Sawyer Hogg 
1969), measures from 62 exposures on 32 of the plates were published. 
The present paper, with results from 51 exposures on 26 plates, com- 
pletes the study. One plate, no. 3753, was not measureable. 

Only sixty-two of the 97 variables were measured. The double 
exposures made measuring difficult in crowded areas and where the 
resolution was insufficient. Of the 62, 61 are of the RR Lyrae type. The 
other is the W Virginis star no. 42, with a period of 25.738 days. (The 
W Virginis, no. 84, was too crowded for measurement.) The stars were 
measured with a Cuffey iris astrophotometer. The photographic 
sequence was derived by converting Arp's (1962) B, V sequence to the 
photographic system. The photographic magnitudes of the 62 variables 
are listed in Table I with the heliocentric Julian days of the observa- 
tions. Attempts were made to determine which of the two exposures 



82 

TABLE I: PHOTOGRAPHIC MAGNITUDES 
Plate Julian Day No. 1 No. 2 No. 3 No. 6 No. 7 No. 8 No. 9 No. 10 No. 11 



3802 


2421424.678 


15.26 


15.42 


15.38 








14.71 


15.09 


15.65 






.680 


15.36 


15.42 


15.36 








14.76 


15.07 


15.70 


15.24 


3804 


.697 


15.69 


15.69 


15.72 


14. 


84 




15.20 


15.09 


15.76 


15.20 




.699 


15.69 


15.91 


15.81 








15.26 


15.00 


15.65 


15.72 


3805 


.716 


15.85 


15.50 


15.85 


14. 


72 


15.77 


14.97 


14.82 


15.69 






.717 


15.81 


15.85 


15.65 








15.30 


14.78 


15.80 




3807 


.733 


15.50 


15.57 


15.50 


14. 


96 


15.57 


15.14 


14.67 


15.77 


15.72 




.735 


15.57 


15.65 


15.45 






15.65 


15.20 


14.59 


15.65 


15.48 


3808 


.749 


15.42 


15.95 


15.62 


14. 


76 


15.20 


15.33 


14.57 


15.91 


15.24 




.750 


15.54 


15.66 


15.50 






15.05 


15.40 


14.62 


15.69 


15.48 


3810 


.769 


15.54 


15.91 


15.57 






14.45 


15.38 


14.59 


15.70 


15.50 




.771 




15.91 


15.69 






14.50 


15.42 


14.65 


15.68 


15.72 


3811 


.785 


15.76 


15.69 


15.69 






14.38 


15.45 


14.74 


15.80 


15.50 




.787 


15.85 


15.76 


15.69 






14.38 


15.45 


14.76 


15.99 


15.42 


3813 


.803 


15.81 


15.60 


15.65 






14.55 


15.54 


14.73 


15.80 


15.54 




.805 


15.65 


15.57 


15.45 






14.53 


15.38 


14.84 


15.72 


15.38 


3814 


.820 












14.73 


15.48 


14.91 








.821 












14.78 


15.60 


14.91 


15.6 


15.54 


3816 


.842 






















3817 


25.679 


15.38 


15.72 


15.36 


14. 


90 


15.85 


14.78 


15.33 


15.73 


15.00 




.681 


15.33 


15.57 


15.33 






15.77 


14.62 


15.28 


15.75 


15.05 


3819 


.697 


15.50 


15.50 


15.42 


15. 


15 


15.79 


14.77 


15.40 




14.95 




.699 


15.47 


15.45 


15.38 






15.85 


14.71 


15.28 




15.02 


3820 


.713 


15.60 


15.72 


15.30 


15. 


07 




14.82 


15.33 


15.73 


14.95 




.715 


15.54 


15.69 


15.38 






15.89 


14.87 


15.33 


15.85 


15.14 


3822 


.735 


15.57 


15.65 


15.40 


15. 


15 


15.38 


14.87 


15.40 


15.88 


15.20 




.737 


15.85 


15.62 


15.40 






15.33 


14.89 


15.33 


15.85 


15.11 


3823 


.751 


15.57 


15.65 


15.57 


15. 


12 


14.73 


15.26 


15.38 


15.85 


15.20 




.753 


15.57 


15.60 


15.40 


14. 


98 


14.65 


14.98 


15.33 


15.77 


15.17 


3825 


.772 


15.76 


15.57 


15.42 


15. 


09 


14.30 


15.07 


15.36 


15.62 


15.24 




.774 


15.60 


15.72 


15.40 






14.30 


15.02 


15.42 


15.70 


15.33 


3826 


.794 


15.69 


15.85 


15.57 


15. 


05 


14.59 


15.24 


15.42 


15.65 


15.22 




.796 


15.60 


15.76 


15.45 






14.59 


15.36 


15.45 


15.65 


15.30 


3828 


.815 


15.60 


15.62 


15.60 


15. 


09 


14.84 


15.42 


15.62 


15.75 






.818 


15.72 


15.57 


15.50 






14.78 


15.48 


15.57 


15.77 


15.40 


3830 


26.705 


15.33 


15.60 


15.12 


15. 


15 


15.85 


15.65 


15.76 


15.57 






.707 


15.30 


15.45 


15.02 






15.70 


15.57 


15.62 


15.57 


14.73 


3832 


.721 


15.38 


15.40 


15.02 


15. 


09 


15.42 


15.42 


15.54 


15.80 


14.24 




.723 


15.26 


15.45 


14.84 






15.45 


15.22 


15.62 


15.70 


14.26 


3833 


.758 


15.57 


15.72 


14.82 


15. 


00 


14.36 


14.67 


15.42 


15.61 


14.34 




.762 


15.60 


15.62 


14.82 






14.40 


14.73 


15.36 


15.70 


14.51 


3835 


.777 






15.22 






14.67 


14.67 


15.60 


15.90 


14.65 




.778 






15.24 








14.86 


15.20 


15.64 


14.80 


3836 


.793 


16.00 




15.30 






14.88 


15.05 


15.48 




14.67 




.794 


15.81 




15.14 






14.80 


15.05 


15.17 


15.77 


14.57 


3837 


.801 


16.00 




15.20 






14.65 


14.95 


15.22 


15.85 


14.80 




.803 


16.00 




15.22 






14.74 


14.95 


15.11 


15.90 


14.69 


3838 


.810 


15.76 


15.30 


15.12 


15. 


28 


14.88 


14.95 


14.82 


16.00 


14.71 




.812 


15.81 


15.72 


15.05 






15.00 


14.97 


14.84 


15.66 


14.71 


3866 


54.721 
.723 























83 



No. 12 No. 14 No. 15 No. 16 No. 18 No. 19 No. 20 No. 21 No. 25 No. 28 No. 29 



14.84 


15.20 


14.86 




14.22 


14.62 


14.74 




14.40 






14.95 


14.82 


15.28 


14.84 




14.40 


14.65 


14.82 




14.36 






15.07 


15.12 


14.76 


15.17 


15.30 


14.50 


14.97 


14.69 


15.57 


14.27 






15.09 


15.24 


14.89 


15.05 


15.14 


14.84 


14.97 


14.69 


15.65 


14.35 






15.26 




14.38 


14.99 


15.32 


14.78 


15.00 


14.48 


15.65 








15.26 




14.40 


15.05 


15.23 


14.73 


15.17 


14.55 


15.54 








15.40 


15.22 


14.57 


14.99 


15.16 


14.67 


15.02 


14.71 


15.57 


14.35 


15. 


65 


15.50 


15.20 


14.48 


14.91 


14.97 


14.71 


15.00 


14.74 


15.28 


14.27 


15. 


62 


15.42 


15.40 


14.53 


15.09 


15.18 


14.93 


15.30 


14.76 


15.77 


14.32 






15.26 


15.42 


14.65 


15.09 


15.04 


14.86 


15.30 


14.76 


15.66 


14.25 


15. 


48 


15.69 


15.36 


14.71 


15.17 


15.30 


15.00 


15.30 


14.95 


15.70 


14.50 


15. 


07 


15.66 


15.54 


14.80 


15.26 


15.30 


15.09 


15.54 


15.02 


15.80 


14.52 


15. 


17 


15.69 


15.42 


14.84 


15.42 


15.28 


15.22 


15.44 


14.97 


15.85 


14.44 


14. 


82 


15.50 


15.38 


14.86 


15.48 


15.32 


15.30 


15.72 


14.89 


15.85 


14.54 


14. 


82 


15.57 


15.54 


15.02 


15.42 


15.32 




15.54 


14.93 


15.77 


14.44 


14. 


57 


15.65 


15.44 


15.02 


15.42 


15.28 




15.50 


14.95 


15.69 


14.43 






15.60 


15.47 


15.11 


15.62 


15.44 


15.48 




15.07 


15.57 


14.59 


14. 


71 




15.50 


15.05 


15.65 


15.26 


15.40 




15.05 


15.54 


14.52 


14. 


69 




15.30 


14.67 


15.07 


14.59 


15.07 


15.36 


15.60 


15.42 


14.32 


15. 


80 


15.57 


15.22 


14.57 


15.02 


14. 35 


14.98 


15.30 


15.54 


15.40 


14.27 


15. 


69 


15.65 


15.28 


14.36 


14.97 


14.14 


15.12 


15.48 


15.38 


15.60 


14.41 


15. 


70 


15.50 


15.24 


14.32 


15.02 


14.02 


15.02 


15.50 


15.40 


15.50 


14.32 


15. 


66 


15.50 


15.44 


14.50 


15.05 


14.16 


15.12 


15.62 


15.42 


15.50 


14.39 


15. 


80 


15.88 


15.38 


14.45 


15.05 


14.04 


15.20 


15.60 


15.54 


15.42 


14.41 


15. 


69 


15.70 


15.48 


14.65 


15.02 


14.18 


15.33 


15.54 


15.50 


15.48 


14.37 


15. 


69 


15.72 


15.45 


14.69 


15.14 


14.18 


15.33 


15.69 


15.57 


15.44 


14.41 


15. 


65 


15.65 


15.54 


14.78 


15.20 


14.20 


15.50 


15.85 


15.57 


15.69 


14.44 


15. 


75 


15.77 


15.50 


14.71 


15.14 


14.18 


15.44 


15.76 


15.45 


15.57 


14.35 


15. 


63 


15.73 


15.64 


14.86 


15.24 


14.38 


15.57 


15.76 


15.72 


15.81 


14.41 


15. 


75 


15.77 


15.70 


15.00 


15.20 


14.30 


15.57 


15.85 


15.76 


15.57 


14.43 


15. 


70 


15.80 


15.80 


14.91 


15.38 




15.65 


15.72 


15.69 


15.69 


14.46 


15. 


75 


15.95 


15.67 


15.00 


15.40 


14.36 


15.57 


15.85 


15.88 


15.69 


14.50 


15. 


64 


15.77 


15.80 


15.20 


15.65 


14.49 


16.00 


15.88 


15.62 


15.66 


14.52 






15.71 


15.70 


15.17 


15.54 


14.52 


16.00 


15.85 


15.69 


15.70 


14.48 






15.69 


15.62 


14.67 


15.05 


15.26 


15.65 


15.62 


15.20 


14.55 


14.35 


15. 


69 


15.73 


15.60 


14.73 


15.00 


15.26 


15.40 


15.57 


15.17 


14.53 


14.32 


15. 


54 


15.71 


15.57 


14.67 


15.07 


15.38 


15.88 


15.88 


15.26 


14.59' 


14.39 


15 


80 


15.69 


15.66 


14.57 


15.05 


15.2 


15.62 


15.72 


15.17 


14.57 


14.37 


15 


66 


15.71 


15.73 


14.89 


15.14 


15.35 


15.91 


15.72 


15.38 


14.84 


14.41 


15 


72 


15.72 


15.85 


15.00 


15.14 


15.28 


15.95 


15.65 


15.24 


14.84 


14.39 


15 


57 


15.60 


16.00 


14.91 


15.44 




16.00 




15.26 


15.14 


14.67 








15.68 


15.02 


15.62 




16.00 


15.81 


15.14 


15.07 


14.61 








15.69 


15.14 






16.00 






15.57 


14.65 








15.40 


,14.91 


15.33 




16.00 


16.0 




15.20 


14.50 










15.36 


15.65 




16.00 


15.95 




15.40 


14.44 










15.14 


15.45 




16.00 


16.04 




15.28 


14.32 








16.00 


15.17 


15.54 




16.00 


15.91 


15.42 


15.12 


14.56 






15.3 


16.00 


15.24 


15.50 




16.00 


16.08 


15.48 


15.12 


14.54 






15.17 



84 



Julian Day No. 30 No. 31 No. 32 No. 33 No. 35 No. 38 No. 39 No. 40 No. 41 No. 42 



2421424 



25 



26 



54 



678 
680 
697 
699 
716 
717 
733 
735 
749 
750 
769 
771 
785 
787 
803 
805 
820 
821 
842 
679 
681 
697 
699 
713 
715 
735 
737 
751 
753 
772 
774 
794 
796 
815 
818 
705 
707 
721 
723 
758 
762 
777 
778 
793 
794 
801 
803 
810 
812 
721 
723 



15.48 
15.50 
15.44 
15.57 
15.42 
15.24 
15.50 
15.42 
15,54 
15.62 
15.57 
15.57 
15.50 
15.47 
15.72 
15.60 

15.14 
14.95 
14.91 
14.74 
14.82 
14.76 
14.86 
14.84 
15.00 
14.95 
15.02 
15.00 
15.17 
15.12 
15.26 
15.26 
15.72 
15.57 
15.75 
15.63 
15.65 
15.65 
15.65 
15.75 
15.75 
15.57 
15.73 
15.63 



15.62 
15.57 
15.48 
15.42 
15.40 
15.26 
15.40 
15.42 
15.42 
15.48 
15.30 
15.40 
15.02 
15.02 
15.07 
14.91 

15.48 
15.42 
15.22 
15.12 
14.97 
14.89 
14.93 
14.95 
14.91 
14.95 
14.88 
14.88 
15.00 
14.97 
15.12 
15.14 
14.95 
15.00 
15.17 
15.14 
15.30 
15.26 

15.57 

15,65 
15.65 

15.85 
15.69 



14.84 
14.86 
14.65 
14.59 
14.05 
14.26 
14.28 
14.30 
14.53 
14.53 
14.69 
14.80 
14.86 
14.95 
15.07 
14.97 
15.22 
15.38 

14.67 
14.78 
14.89 
14.78 
15.00 
14.97 
15.09 
15.20 
15.38 
15.26 
15.42 
15.42 
15.57 
15.48 
15.72 
15.69 
15.44 
15.44 
15.69 
15.48 
15.69 
15.81 
15.85 
16.00 

15.85 
16.00 
15.96 



14.82 
14.84 
14.91 
14.89 
15.00 
15.20 
15.26 
15.07 
15.22 
15.20 
15.36 
15.33 
15.40 
15.36 
15.44 
15.42 



14.88 
14.91 
14.93 
15.00 
14.95 
15.02 
15.17 
15.12 
15.26 
15.07 
15.33 
15.17 
15.12 
15.24 
15.40 
15.44 
15.00 
14.91 
15.17 
14.91 
15.24 
15.22 



15.22 
15.36 



15.20 
15.40 
15.28 
15.40 
15.13 
15.08 
15.06 
15.00 

15.13 

15.18 
14.82 
14.82 

14.71 



15.19 
15.06 
15.10 
15.00 
15.02 
14.87 
14.71 
14.64 
14.56 

14.68 
14.58 
14.58 
14.60 
14.64 
14.75 
14.56 
14.68 
14.57 
14.73 
14.68 

14.94 

15.00 
14.97 
14.91 



15.48 15.08 



15.65 
15.62 

15.45 
15.65 

15.54 



15.70 



15.60 
15.67 
15.54 

15.62 
15.62 
15.60 
15.62 
15.48 
15.48 
15.60 
15.70 
15.65 
15.60 
15.60 
15.30 
15,62 



14.73 
14.59 
14.76 
14.67 
14.26 
14.20 



15.36 
15,57 
15.60 
15.48 
15,44 
15.40 
15.57 
15.54 
15.81 
15.81 
15.75 
15.80 
15.72 
15.65 



15.36 
15.28 
15.40 
15.30 
15.42 
15.44 
15.44 
15.54 
15,62 
15.50 
15.54 
15.54 
15.62 
15.62 
15.76 
15.62 
14.57 
14.53 
14.67 
14.55 
14.89 
14,89 
14,80 
14,86 
14,82 
14.69 



15.09 
15.26 



15.12 
15.00 
15.09 
15.11 
14.95 
15.02 
14.89 
14.73 
14.78 
14.82 
14.95 
14.91 
14.93 
14.97 
14.97 
14.93 
15.18 
15.12 

14.91 
14.97 
14.84 
14.95 
14.84 
14.93 
14.82 
14.89 
14.86 
14.95 
14.95 
14.93 
15.09 
15.07 
15.24 
15.26 
14.89 
14.93 
15.02 
15.00 
15.14 
15.24 



15.42 
15.50 
15.52 
15.62 
15.50 



15.36 
15.36 
15.26 
15.26 
15.30 
15.40 
15.48 
15.48 
15.48 
15.38 
15.72 
15.65 
15.70 
15.70 
15.81 
15.62 



15.30 
15.42 
15.57 
15.57 
15.42 
15.40 
15.62 
15.69 
15.72 
15.60 
15.72 
15.72 
15.60 
15.69 
15.75 
15.66 
15.50 
15.50 
15.65 
15.62 
15.81 
15.50 



16.00 
15.69 
15.68 
15.75 
15.78 
15.66 



12.10 



12.20 
12.10 
11.95 
11.75 
11.85 
11.75 
12.15 

12.15 
12.05 
12.15 
12.05 
12.20 
12.00 
11.85 
12.00 
12.25 
12.05 
12.15 
12.35 
12.20 
12.00 
12,20 



85 

No. 43 No. 44 No. 45 No. 47 No. 52 No. 55 No. 58 No. 59 No. 61 No. 62" No. 63 



15.22 


14.65 




15.00 


14.55 




14.86 


15.05 


15.38 




15.17 


15.12 


14.76 




15.07 


14.80 




14.84 


15.07 


15.36 




15.20 


14.76 


14.89 


15.72 




15.09 






14.93 


15.70 


15.62 


15.62 


14.95 


14.89 


15.60 




15.40 


14.97 


14.59 


15.07 


15.77 


15.70 


15.54 


14.84 


15.02 


15.70 




15.14 


15.00 


14.55 


14.53 


15.73 


15.26 


15.57 


14.97 


15.05 


15.95 




15.30 


15.02 


14.89 


14.50 


15.85 


15.38 


15.65 


15.05 


15.22 


15.70 




15.24 


15.12 


15.24 


14.59 


15.65 


15.14 


15.40 


15.07 


15.20 


15.73 


15.38 


15.30 


14.91 


15.22 


14.56 


15.65 


15.00 


15.36 


15.05 


15.17 


15.65 


15.50 


15.38 


14.86 


15.28 


14.50 


15.75 


15.02 


15.68 


14.93 


15.12 


15.57 


15.57 


15.28 


14.95 


15.57 


14.84 


15.67 


14.91 


15.75 


15.09 


15.22 


15.60 


15.54 


15.42 




15.72 


14.80 


15.80 


14.91 


15.65 


15.17 


15.14 


15.65 


15.48 


15.44 


15.05 


15.69 


14.91 


15.75 


15.05 


15.70 


15.17 


15.20 


15.36 




15.44 




15.62 


14.74 


15.69 


14.91 


15.75 


15.12 


15.17 


15.33 


15.57 


15.37 


15.24 


15.65 


14.84 


15.72 


14.88 


15.85 


15.26 


15.50 


14.76 


15.42 


15.40 






14.89 


15.65 


14.88 


15.70 


15.22 


15.17 


14.93 


15.42 


15.50 


15.22 


15.69 


14.95 


15.57 


14.86 


15.68 


15.26 


15.22 


14.78 










15.02 


15.72 


15.05 


15.73 


15.26 


15.22 


14.78 






15.38 




15.00 


15.50 


15.00 


15.66 


15.60 


14.82 


15.22 


15.28 


15.14 




15.02 


15.48 


15.05 


15.07 


15.50 


15.60 


14.80 


15.24 


15.14 


15.16 


15.02 


15.00 


15.54 


15.09 


15.14 


15.62 


15.57 


14.80 


15.22 


15.30 


15.22 




14.86 


15.57 


14.93 


15.20 


15.75 


15.50 


14.78 


15.30 


15.17 


15.38 


14.89 


14.93 


15.50 


14.97 


15.17 


15.65 


15.54 


14.91 


15.17 


15.26 


15.24 


14.93 


15.28 


15.72 


15.14 


15.26 


15.68 


15.57 


14.82 


15.24 


15.22 


15.33 


15.02 


15.22 


15.76 


15.17 


15.30 


15.73 


15.69 


14.95 


15.33 


15.33 


15.30 




15.28 


15.65 


15.20 


15.33 


15.62 


15.57 


14.89 


15.24 


15.28 


15.50 


14.95 


15.28 


15.60 


15.14 


15.44 


15.77 


15.54 


14.95 


15.22 


15.40 


15.38 


15.17 


15.42 


15.48 


15.30 


15.60 


15.68 


15.36 


14.97 


15.24 


15.36 


15.42 


15.09 


15.42 


15.42 


15.22 


15.57 


15.66 


15.54 


15.30 


15.40 


15.48 


15.44 




15.54 


14.84 


15.28 


15.67 


15.65 


15.62 


15.12 


15.33 


15.48 


15.50 


15.05 


15.62 


14.88 


15.36 


15.69 


15.70 


15.44 


15.14 


15.20 


15.40 


15.44 


15.20 


15.76 


14.53 


15.48 


15.70 


15.65 


15.42 


15.12 


15.24 


15.36 


15.62 


15.14 


15.85 


14.42 


15.42 


15.70 


15.75 


15.72 


15.22 


15.30 


15.54 


15.55 




15.69 


14.42 


15.54 


15.60 


15.77 


15.60 


15.22 


15.28 


15.38 


15.55 


15.46 


15.69 


14.48 


15.42 


15.54 


15.80 


15.02 


14.80 


14.38 


14.93 


15.20 


15.12 


15.38 


15.57 


15.20 


15.20 


15.57 


15.00 


14.80 


14.53 


14.89 


15.26 


14.95 


15.24 


15^.50 


15.14 


15.12 


15.57 


15.00 


14.89 


14.50 


15.02 


15.36 


15.02 


15.42 


15.57 


14.65 


15.00 


15.66 


15.00 


14.91 


14.42 


15.00 


15.34 


15.00 


15.33 


15.57 


14.62 


15.00 


15.68 


15.14 


15.17 


14.65 




15.38 




15.50 


15.50 


14.73 


14.86 


15.73 


15.17 


15.12 


14.71 


15.22 


15.60 


15.14 


15.42 


15.48 


14.78 


14.86 


15.70 


15.07 














15.65 


15.00 




16.00 


15.14 










15.42 




15.48 


14.71 


14.97 


15.85 


15.17 














15.50 


14.65 


15.26 


16.00 


15.00 


15.42 




15.40 




15.36 




15.40 


14.57 


15.09 


15.90 


15.20 


15.57 












15.22 


14.53 


15.22 


15.90 


15.20 


15.57 








15.42 




15.22 


14.57 


15.24 


15.85 


15.09 


15.65 


15.09 








15.69 


15.90 


14.91 


15.26 


15.90 


15.12 


15.50 


14.95 






15.65 


15.88 


15.77 


15.02 


15.22 


15.90 



86 

Julian Day No. 64 No. 65 No. 66 No. 67 No. 68 No. 69 No. 70 No. 71 No. 72 No. 73 



2421424 



25 



26 



678 
680 
697 
699 
716 
717 
733 
735 
749 
750 
769 
771 
785 
787 
803 
805 
820 
821 
842 
679 
681 
697 
699 
713 
715 
735 
737 
751 
753 
772 
774 
794 
796 
815 
818 
705 
707 
721 
723 
758 
762 
777 
778 
793 
794 
801 
803 
810 
812 



15.72 
15.72 
15.72 
15.60 
15.57 
15.50 
15.76 
15.48 
15.67 
15.73 
15.75 
15.73 
15.67 
15.48 



15.50 
15.38 
15.50 
15.40 
15.68 
15.65 
15.76 
15.62 
15.73 
15.65 
15.75 
15.75 
15.70 
15.64 
15.77 
15.77 
15.28 
15.20 
15.26 
15.17 
15.42 
15.28 
15.22 
15.38 
15.44 
15.24 



15.68 
15.50 



15.67 
15.70 
15.85 
15.88 
15.75 
15.48 
15.95 
15.60 
15.86 
15.80 
15.65 
15.62 
15.60 
15.57 



15.65 
15.69 
15.57 
15.69 
15.78 
15.73 
15.36 
15.88 
15.69 
15.70 
15.62 
15.89 
15.65 
15.75 
15.60 
15.77 
15.50 
15.75 
15.65 
15.73 
15.48 
15.85 
15.57 
15.20 
14.84 
14.76 
14.76 
14.89 
14.74 



15.26 
15.50 
15.48 
15.33 
15.69 
15.50 
15.42 
15.65 
15.70 
15.70 
15.54 
15.65 



15.22 
15.20 
15.30 
15.30 
15.22 
15.20 
15.33 
15.36 
15.50 
15.48 
15.48 
15.44 
15.44 
15.54 
15.63 
15.70 
14.91 
14.89 
15.14 
15.12 
15.12 
15.17 
14.91 
15.30 

15.50 
15.60 
15.64 
15.57 
15.62 



14. 
14. 
14. 
14. 
14. 
14. 
14. 
15. 
15. 
15. 
15. 
15. 
15. 
15. 
15. 
15. 



40 
40 
38 
35 
30 
38 
86 
02 
07 
00 
17 
30 
38 
40 
38 
28 



16.00 



14. 
14. 
14. 
14. 
14. 
14. 
14. 
14. 
14. 
14. 
15. 
15. 
15. 
15. 
15. 
15. 
15. 
15. 
14. 
14. 
14. 
14. 
14. 
14. 
14. 
14. 
14. 
14. 



73 
78 
84 
80 
53 
65 
73 
67 
84 
82 
07 
14 
12 
00 
54 
44 
38 
28 
69 
59 
30 
30 
36 
32 
30 
30 
48 
65 



14.59 
14.93 
15.17 
15.17 
15.85 
15.48 



15.17 
15.24 
15.42 
15.48 
15.50 
15.42 
15.48 
15.42 
15.80 
15.75 
15.73 
15.67 
15.85 
15.80 



15.50 
15.48 



15.90 
15.90 



15.30 




14.24 


15.23 


15.36 




14.36 


15.23 


14.71 


15.66 


14.30 




14.86 


15.90 


14.30 




15.17 


15.70 


14.30 


14.80 


15.36 


15.90 


14.30 


14.97 


15.36 


15.75 


14.32 


15.22 


15.60 


15.60 


14.57 


15.14 


15.76 


15.95 


14.59 


15.30 


15.54 


15.77 


14.67 


15.28 


15.48 




14.91 


15.33 


15.69 




15.07 


15.45 


15.87 


16.00 


15.36 


15.72 


15.73 




15.36 


15.60 


15.87 




15.54 


15.72 


15.65 




15.38 


15.60 



15.28 
15.36 
15.30 
14.73 
14.78 
14.74 
14.74 
15.00 
14.78 
15.12 
15.05 
15.26 
15.24 
15.42 
15.36 
16.00 
15.90 
15.90 
15.98 
15.95 
15.95 



15.57 
15.48 
15.64 
15.33 
15.20 



15.85 



16.00 
16.00 



16.00 
15.95 



15.95 
15.77 



16.00 
16.00 



15.20 
15.07 
14.36 
14.38 
16.00 
15.95 



15.92 
16.00 



14.59 
14.84 
14.95 
14.97 
15.02 
15.02 
14.93 
15.07 
15.20 
14.88 
15.24 
15.36 
15.42 
15.42 
15.60 
15.48 
14.84 
14.84 
15.00 
15.05 
14.97 
15.02 
14.86 
14.82 
15.48 
15.30 
15.36 
15.30 
15.24 
15.30 



87 

No. 74 No. 75 No. 76 No. 77 No. 78 No. 79 No. 80 No. 81 No. 83 No. 87 No. 92 









14.73 


15.20 


14.89 


14.78 


14.57 














14.74 


15.38 


14.89 


15.20 


14.46 








13.90 


14.71 


14.50 


14.89 


15.24 




14.91 


15.12 




15.02 




13.90 


14.89 


14.67 


15.07 


15.36 




15.33 


14.76 


15.85 


15.26 


14.54 


13.90 


14.69 


14.67 


14.93 


15.09 


15.38 


14.88 


14.93 


15.77 


14.91 


14.70 


13.90 


14.89 


14.57 


14.93 


15.24 


15.38 


15.50 


14.78 


15.75 


15.17 


14.77 


13.90 


15.00 


14.71 


14.91 


15.00 


15.07 


15.00 


15.02 


15.77 


14.93 


14.42 


13.90 


14.89 


14.78 


14.91 


15.05 




15.20 


14.73 


15.77 


14.95 


14.44 


13.90 


15.24 


14.76 


15.07 


14.84 


15.22 


14.71 


15.00 


15.72 


14.89 


14.09 


13.92 


15.17 


14.74 


15.00 


14.97 


15.09 


15.07 


14.80 


15.36 


14.93 


14.57 


13.91 


15.26 


14.82 


14.97 


14.82 


15.14 


14.74 


15.17 


15.64 


14.91 


14.72 


13.98 


15.30 


14.95 


15.09 


15.05 


15.22 


15.02 


15.09 


15.62 


15.05 


14.72 


14.18 


15.36 


14.93 


15.09 


14.97 


15.00 


14.84 


15.17 


15.60 


15.02 


14.40 


14.24 


15.28 


15.05 


15.09 


14.95 




15.05 


15.17 


15.60 


15.07 


14.38 


14.10 


15.30 


15.05 


15.02 


15.12 


14.95 


14.76 


15.24 


15.64 


14.91 


14.38 


14.30 


15.28 


14.95 


15.07 


15.00 


14.84 


14.91 


15.09 


15.46 


15.02 


14.07 


14.36 


15.38 


15.09 


15.17 


15.12 


15.00 




15.26 




15.02 


14.22 


14.32 




15.20 


15.09 


15.14 


14.93 




15.30 


15.50 


15.09 


14.57 


14.02 


15.57 


15.09 


15.09 


15.30 


15.24 


15.07 


15.75 


15.40 


15.17 


14.48 


13.96 


15.65 


15.02 


15.24 


15.33 


15.12 


15.36 


15.55 


15.36 


15.26 


14.30 


14.16 


15.69 


14.89 


15.14 


15.44 


15.36 


15.02 


15.85 


15.48 


15.17 


14.26 


14.18 


15.57 


15.02 


15.17 


15.48 


15.22 


15.36 


15.60 


15.50 


15.28 


14.07 


13.98 


15.81 


15.22 


15.20 


15.38 


15.36 


14.82 


15.73 


15.57 


15.17 


14.65 


14.14 


15.76 


15.30 


15.22 


15.38 


15.40 


15.26 


15.54 


15.60 


15.22 


14.42 


14.04 


15.60 


15.26 


15.12 


15.36 


15.33 


14.91 


15.07 


15.50 


15.14 


14.76 


14.00 


15.62 


15.24 


15.24 


15.42 


15.17 


15.20 


14.95 


15.57 


15.26 


14.40 


14.16 


15.76 


15.30 


15.20 


15.33 


15.24 


14.78 


14.95 


15.50 


15.22 


14.22 


14.08 


15.81 


15.24 


15.22 


15.26 


15.26 


14.97 


14.74 


15.57 


15.20 


14.12 


14.12 


15.73 


15.30 


15.17 


15.17 


14.97 


14.67 


14.48 


15.60 


15.24 


14.40 


14.18 


15.80 


15.36 


15.12 


15.07 


14.97 


14.97 


14.38 


15.48 


15.24 


14.38 


14.20 


15.77 


15.40 


15.28 


14.89 


14.89 


14.65 


14.57 


15.50 


15.30 


14.00 


14.24 


15.73 


15.38 


15.30 


14.95 


15.00 


14.88 


14.65 


15.57 


15.36 


14.02 


14.30 


15.73 


15.57 


15.40 


14.93 


14.93 


14.74 


14.78 


15.54 


15.38 


13.50 


14.28 


15.77 


15.48 


15.33 


14.97 


14.91 


14.84 


14.74 


15.44 


15.60 


13.34 


14.28 


15.02 


15.24 


15.28 


15.20 


15.28 




15.72 


15.02 


15.38 


14.07 


14.12 


14.95 


15.20 


15.36 


15.22 


15.20 


15.28 


15.42 


15.14 


15.40 


14.17 


14.16 


15.12 


15.36 


15.26 


15.26 


15.30 


14.97 


15.70 


15.20 


15.36 


14.00 


14.26 


15.07 


15.24 


15.26 


15.44 


15.17 


15.38 


15.48 


15.24 


15.38 


13.97 


14.24 


15.07 


15.00 


15.38 


15.40 


15.07 


14.89 


15.60 


15.36 


15.24 


13.18 


14.18 


15.02 


14.91 


15.36 


15.40 


15.17 


15.14 


15.65 


15.28 


15.12 


13.34 


14.26 


15.26 




15.44 


15.80 


15.44 






15.77- 




13.62 


14.26 


15.14 




15.26 


15.65 


15.20 




15.72 


15.73 




13.26 




15.20 


15.09 




15.68 


15.07 


15.00 




15.69 




13.73 




15.07 


14.95 




15.68 


14.74 


15.14 




15.60 




13.60 




15.20 


14.95 




15.67 


14.76 






15.60 




13.91 




15.14 


15.05 




15.80 


14.80 










13.70 


14.18 


15.40 


14.97 


15.48 


15.50 


15.02 


14.82 




15.92 




14.02 


14.22 


15.44 


14.97 


15.50 


15.48 


15.02 


14.97 




15.76 




13.93 



88 



Christine M. Coutts 





VI 


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Variables in Mo: A Study of Mount Wilson 1917 Observations 89 



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90 



Christine M. Coutts 



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Fig. 1, cont'd — Light Curves of the 62 Variables. 



Variables in M5: A Study of Mount Wilson 1917 Observations 91 



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92 



Christine M. Coutts 



160 

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Fig. 1, cont'd — Light Curves of the 62 Variables. 



Variables in M5: A Study of Mount Wilson 1917 Observations 93 



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I5.5^«\.. • 



• .•^^' • ..' 



V87 ••• ., P=0-74 

^ • • • • • • 



• '• • • 



-I • • • «• 



150 



■5 5 5 -5 

Fig. 1, cont'd — Light Curves of the 62 Variables. 



94 



Christine M. Coutts 



TABLE II 
Elements of the Variables 





Epcx;h 






Comments 


Var. 


of Max. 


Period 


/3 


on Period 


1 


21424.976 


0.5217856 




const 


2 


21424.886 


0.526 






3 


21424.937 


0.6001832 


0.04 




6 


21424.744 


0.5488311 


-0.05 




7 


21424.779 


6.4943896 


0.07 




8 


21424.575 


0.546224 


0.09 




9 


21424.739 


0.698895 




const 


10 


21424.852 


0.5306628 


-0.02 




11 


21424.943 


0.5958914 




const 


12 


21424.621 


0.4677144 


-0.06 




13 




0.5131223 


0.04 




14 


21424.726 


0.4872423 






16 


21424.693 


0.3367607 


0.03 




16 


21424.406 


0.6476223 


0.12 




18 


21424.631 


0.46388 






19 


21424.603 


0.4699535 


0.16 




20 


21424.699 


0.6094759 




const 


21 


21424.876 


0.6048941 




const 


25 


21424.525 


0.508 






27 




0.4703 






28 


21424.805 


0.5439474 


-0.13 




29 


21424.584 


0.4514334 


-0.12 




30 


21424.518 


0.5921755 




const 


31 


21424.560 


0.3005826 




const 


32 


21424.710 


0.4577863 




const 


33 


21424.616 


0.5014722 


0.04 




34 




0.5681431 




const 


35 


21424.548 


0.3081197 






36 




0.6277229 




const 


38 


21424.927 


0.4704441 






39 


21424.881 


0.5890346 


0.05 




40 


21424.762 


0.3173286 


0.03 




41 


21424.538 


0.4885749 


-0.04 




42 


21418.129 


25.738 




W Virginia 


43 


21424.689 


0.6602264 




const 


44 


21424.643 


0.329 






45 


21424.847 


0.6166364 




const 


47 


21424.978 


0.5397295 


-0.09 




52 


21424.522 


0.5017848 






55 


21424.719 


0.3288968 


0.03 




58 


21424.620 


0.491265 






59 


21424.712 


0.5420259 




const 


61 


21424.456 


0.5686157 


0.10 




62 


21424.789 


0.2814092 






63 


21424.500 


0.4976763 


0.04 




64 


21424.954 


0.5445075 


-0.13 




65 


21424.902 


0.480691 






66 


21424.574 


0.350682 






67 


21424.681 


0.3490462 






68 


21424.647 


0.3342797 






69 


21424.881 


0.4948743 




const 


70 


21424.603 


0.5585255 


0.18 




71 


21424.968 


0.5024676 


0.07 





Variables in M5: A Study of Mount Wilson 1917 Observations 95 



TABLE II — continued 





Epoch 






Comments 


Var. 


of Max. 


Period 


/3 


on Period 


72 


21424.682 


0.562 






73 


21424.626 


0.3401118 


0.05 




74 


21424.667 


0.4539961 


-0.06 




75 


21424.639 


0.6854136 


0.07 




76 


21424.663 


0.432421 


0.03 




77 


21424.521 


0.8451121 


0.11 




78 


21424.760 


0.2648174 




const 


79 


21424.548 


0.3331387 




const 


80 


21424.836 


0.3365424 


-0.02 




81 


• 21424.647 


0.5573235 


-0.18 




83 


21424.955 


0.5533073 




const 


87 


21424.736 


0.7383888 




const 


92 


21424.893 


0.4635789 







Remarks to Table 1 1 
Vars. 13, 27, 34 and 36 were all studied on the David Dunlap plates by Coutts and 
Sawyer Hogg (1969), but were too crowded for measurement on the Mount Wilson 
1917 plates. 

was taken first. Both Dr. Shapley and Miss Henrietta Swope were 
consulted. The latter perused the Mt. Wilson records, but no definite 
decision was made. In constructing the Table it was assumed that the 
later exposure is the one to the west. This point is not of great impor- 
tance because an average of the two was used in forming the light 
curves of the 62 variables which are shown in Figure I. 

The curves, based on observations from eight different nights, are 
well defined and are therefore very useful for any studies of period 
changes of the variables. The periods adopted are the same as those 
used in Coutts and Sawyer Hogg (1969) and are listed in Table H, 
along with the epoch of maximum light for 1917. Also listed is /3, the 
rate of period change, adopted from Coutts and Sawyer Hogg (1969) 
or Coutts (1969). Of the 61 RR Lyrae type stars, 46 are of type a and 
have periods ranging from 0.45 to 0.85 days and median 0.54 days. The 
other 15 are of type c with periods between 0.26 and 0.43 days and 
median 0.33 days. This is the period distribution for a cluster of the 
OosterhofT type I. 



This program has been supported by grants from the National 
Research Council of Canada to Dr. Helen S. Hogg. I am grateful 
to Dr. H. W. Babcock for the loan of the Mt. Wilson plates and to 
Mr. Basil Katem for making the necessary arrangements. It is a 
pleasure to thank Dr. Hogg for her invaluable guidance. 



96 Christine M. Coutts 

References 

Arp, H. 1962, Ap. J., 135, 311. 

Bailey, S. I. 1917, Harvard Ann., 78, 157. 

Coutts, C. 1969, On the Nature of Some of the 0-C Diagrams of the RR Lyrae 

Variables in M5. Non-Periodic Phenomena in Variable Stars. Budapest, Academic 

Press. 
Coutts, C. M. and Sawyer Hogg, H. 1969, David Dunlap Obs. Pub. 3, no. 1. 
Kukarkin, B. V. and Kukarkina, N. P. 1969, Astronomical Circular, no. 541. 
Oosterhoff, P. Th. 1941, Leiden Ann., 17, pt. 4. 
Shapley, H. 1927, Harvard Bull., no. 851, 15. 

Richmond Hill, Ontario 
May 26, 1971 



( 



PUBLICATIONS OF 

THE DAVID DUNLAP OBSERVATORY 

UNIVERSITY OF TORONTO 

Volume 3 Number 4 



SPECTROSCOPIC ORBITS OF THE 

BINARY SYSTEMS 

H.D. 128661, ARCas,pAri and H.D.209813 



WALTER L. GORZA 

AND 

JOHN F. HEARD 




1971 
TORONTO. CANADA 



PUBLICATIONS OF 

THE DAVID DUNLAP OBSERVATORY 

UNIVERSITY OF TORONTO 

Volume 3 Number 4 



SPECTROSCOPIC ORBITS OF THE 

BINARY SYSTEMS 

H.D. 128661, ARCas,pAri and H.D.209813 



WALTER L. CxORZA 

AND 

JOHN F. HEARD 



1971 
TORONTO, CANADA 



PRINTED AT 
THE UNIVERSITY OF TORONTO PRESS 



SPECTROSCOPIC ORBITS OF THE BINARY SYSTEMS 
H.D. 128661, AR Cas, /3 Ari and H.D. 209813 

Bv Walter L. Gorza and John F. Heard 

Abstract 

From spectroscopic observations there have been obtained the orbital elements of 
two eclipsing binary systems (H.D. 128661, AR Cas) and two spectroscopic binaries 
(0 Ari and H.D.. 209813). For one system (H.D. 128661), no solution was previously 
available. The other systems are well known and were investigated for possible 
changes in their orbital elements. There seem to be no changes for AR Cas; a small 
change in the value of the longitude of periastron, w, seems probable for /3 Ari ; and 
there is some evidence of a change in the value of the semi-amplitude, K, for H.D. 
209813. 

I)ilrodiicfion 

The spectrograms used during the present work were all obtahied 
with the 12 A mm dispersion of the all-reflection grating spectrograph 
attached to the 7-4-inch telescope of the David Dunlap Observatory. 
The measurements were carried out on the Grant (AR Cas, /3 x\ri and 
part of H.D. 128661) and Zeiss-Abbe (remaining plates for H.D. 
128661 and H.D. 209813) comparators. Preliminary elements were 
derived by the use of a series of computed velocity-curves drawn by 
R. K. Young (except for /3 Ari, for wliich the Lehmann-Filhes method 
was used). Least-scjuares differential corrections were carried out on all 
the preliminary values by the use of a computer program written by 
D. Hube. The equation of condition derived by Lehmann-Filhes 
(1894) was used for all the systems, except for H.D. 209813 for which — 
its eccentricity, e, being so small — Sterne's (1941) method was used. 
The indicated errors are mean errors. The phases (given in the tables 
and used in the diagrams) are given in days relative to the finally 
adopted value for T, the time of periastron passage. Table IX (see page 
110) shows the wavelengths used in obtaining the radial velocities for 
the four binary s>'stems. 

II.D. 128661 

The variable radial velocity of this star (a = W 33?!, 8 = +36° 22', 

. niptg = 6.97, Sp. = AO) was first observed at the Simeis Observatory. 

Jackisch (1968) foiuid that the star was probably an eclipsing variable 

witli the minimum occurring at J.D. 2438906. 4oo. Another minimum 



100 Walter L.Gorza and John F. Heard 

was observed by Harris (1969) to occur at J.D. 2440362.9070. Fol- 
lowing the report by Jackisch, the star was placed on our observing 
program and altogether 52 spectrograms were obtained between 
February 8, 1969 and April 17, 1970. 

By counting our radial velocity measures with the above-mentioned 
times of minima it was possible to obtain a very accurate period of 
3.33284(2) days. The assumption was made that both minima are 
primary minima. This assumption seems to be justified inasmuch as 
only one component is visil)le on the spectrograms. The differential 
correction was carried out only on five elements, the period being held 
fixed. The observations are listed in Table I. Figure 1 (see page 102) 

TABLE I 
Radial-Velocity Observations of H.D. 128661 



J.D. 


Vo 


Phase from 


0-C 


24400004- 


km /sec 


Final T 


km/sec 


260.827 


-44.6 


0.676 


+0.9 


268.950 


+43.0 


2.133 


+2.7 


269.938 


-77.3 


3.121 


+2.7 


270.928 


-31.2 


0.778 


+0.1 


271.896 


+49.1 


1.746 


+ 1.8 


273.932 


-74.6 


. 449 


+ 1.3 


274.853 


+32.7 


1 . 370 


+0.8 


282.842 


-11.7 


2.694 


+4.3 


283.815 


-86.1 


0.334 


+2.4 


284.778 


+27.1 


1.297 


+0.6 


285.763 


+ 32.8 


2.282 


+2.0 


290.784 


-49.1 


0.637 


+ 1.8 


296.712 


-91.0 


3.232 


+0.9 


307 . 860 


+5.6 


1.049 


+2.8 


317.811 


+0.4 


1.001 


+3.1 


323.882 


-79.2 


. 407 


+ 1.7 


325.618 


+41.0 


2.143 


+ 1.2 


331.735 


+46.9 


l..-)94 


+3.4 


341.647 


+39.2 


1 . 507 


-0.7 


346.732 


-93.1 


3.260 


+ 1.0 


353.593 


-100.6 


0.122 


-0.2 


364.699 


+20.9 


1 . 229 


0.0 


365.588 


+41.9 


2.118 


+0.9 


367.613 


-26.6 


0.811 


+0.3 


368.597 


+48.4 


1.795 


+0.7 


371.620 


+36.4 


1.485 


-2.4 


437.607 


-28.4 


0.815 


-2.1 


438.590 


+46.8 


1.798 


-0.9 


4.")6 . 572 


-78.0 


3.116 


+ 1.4 


458.572 


+46.4 


1.783 


-1.3 


459.583 


-31.8 


2.794 


-0.6 


462.578 


+ 14.8 


2.456 


+0.2 


610.809 


-44.6 


. 709 


-3.8 


625.823 


+ 19.3 


2.392 


-1.9 


625.949 


+ 7.5 


2.518 


0.0 


629.917 


-85.8 


3.1.53 


-1.9 


640 . 822 


-40.2 


0.727 


-1.8 


641.899 


+47.5 


1.804 


-0.3 



spectroscopic Orbits of Four Binary Systems 
TABLE I — continued 



101 



J.D. 


Vo 


Phase from 


0-C 


2440000+ 


km /sec 


Final T 


km/sec 


646.753 


-99.7 


3.325 


-1.5 


646.9.51 


-100.4 


0.190 


-1.9 


6.54.820 


+.32.0 


1.393 


-1.4 


6.55.885 


+ 12.4 


2.4.58 


-2.0 


657 . 907 


+ 12.1 


1.147 


-1.1 


6.58. 874 


+39.9 


2.114 


-1.3 


660.806 


-42.0 


0.714 


-1.8 


664.834 


+32.3 


1.409 


-2.1 


665.785 


+22.7 


2 . 360 


-1.6 


• 673.8.58 


— no 


0.434 


+0.2 


675.792 


+20.8 


2.368 


-2.7 


676.840 


-103.0 


0.083 


-2.4 


689.737 


-62.7 


2.982 


-2.1 


693.743 


-89.2 


0.322 


+0.4 



shows the individual observations and the adopted velocity curve. 
The mean error of a single observation was found to be ±1.8 km/sec. 
Table II lists the pre]iniinar\' and tlie final values for tlie elements. 

TABLE II 
Orbital Elements of H.D. 128661 



Element 


Preliminary 


Final 




P (days) 


3.33284(2) 


3.33284(2) 


T (J.D.) 


2440263.460 


2440263.484 


d= 0.003 


(°) 


165 


166.5 


±0.3 


e 


0.15 


. 137 


±0.005 


K (km/sec) 


75.3 


74.2 


±0.4 


y (km/sec) 


-15.9 


-16.5 


±0.3 


a sin i (10%m) 




3.37 


±0.02 


f(m) O 




0.137 


±0.002 



H.D. 221253 (AR Cas) 

AR Cas (a = 23"" 25'?4, 5 = +58° 00', mp,g = 4.89, Sp. = B.3 \') was 
first observed to be a spectroscopic binary by Frost and Adams (1903). 
Photoelectric observations, first by Stebbins (1921), and then b\- 
Huffer and Collins (1962), show a similar value for the longitude of 
periastron, co, while spectroscopic observations first by Baker (1909), 
then by Luyten, Struve and Morgan (1939) and Petrie (1944, 1962), 
show a changing value for cc, which would indicate a rotation of the 
line of apsides (Petrie, 1944). 

Following receipt of Circular Xo. 1 for the "AR Cassiopeiae Co- 
ordination Programme", 44 spectrograms were here obtained between 
August 14, 1968 and September 12, 1969. The period of the system 



102 



Walter L. Gorza and John F. Heard 



60 


- 






40 


- 


0^.,^ \ 


KD. 128661 


20 


- 




k 


Mo 
(km/sec)Q 


- 




\ 


-20 


- 




\ 


-40 


/ 




\ / 


-60 


/ 




\ / 


-80 


/ 




\ / 


-100 


o 

1 


1 1 1 


0^ 

1 1 1 1 



0-0 0-5 



1-0 



3-0 



35 



1-5 2 ^5 

Phase (days) 

Fig. 1— Velocity Curve for the Eclipsing Binary H.D. 12S6G1 



40 



being known with great accuracy, it was held constant while the 
differential correction was carried out on the remaining five elements. 
The residuals were found to be reasonable except for those of three 
observations, which were made close to the time of the primary eclipse. 
It was easy to see that the radial velocities obtained at those points 
could have been innuenced by the rotational velocity of the star itself 
(Batten, 1901), and accordingly they were removed. A new differential 
correction produced the final elements shown in Table IV. The observa- 
tions are listed in Table III. I'igure 2 shows the individual observations 

TABLE III 
Radial-Velocity Observations of AR Cas 



J.D. 


Vo 


Phase from 


0-C 


2440000 + 


km /sec 


Final T 


km /sec 


82.730 


-54. S 


1.603 


-2.8 


83.716 


-56.1 


2.589 


+0.3 


84.590 


-42.6 


3.463 


-2.7 


95.773 


-57.6 


2.513 


-0.5 


98.706 


+45.6 


5.446 


-3.4 


100.825 


-52.3 


1.499 


-2.9 


102.925 


-29.5 


3.599 


+6.4 


103.710 


-5.9 


4.384 


-0.5 


104.849 


+51.1 


5.523 


-0.5 



spectroscopic Orbits of Four Binary Systems 103 

TABLE III — continued 



J.D. 


Vo 


Phase from 


0-C 


2440000+ 


km /sec 


Final T 


km /sec 


106.827 


-49.7 


1.435 


-2.2 


107.731 


-61.4 


2.339 


-3.3 


108.693 


-43.1 


3.301 


+ 1.1 


111.812 


+21.3 


0.353 


0.0 


113.900 


-53.4 


2.441 


+4.2 


1 14.824 


-46.7 


3.365 


-4.2 


120.601 


-52.6 


3.076 


-3.4 


121.747 


-11.7 


4.222 


+ 1.1 


131.656 


-56.2 


1.998 


+ 1.4 


• 143.671 


-57.5 


1.881 


-0.9 


145.712 


-32.3 


3.922 


-7.3 


151.685 


-27.9 


3.828 


+0.5 


161.676 


-54.5 


1.687 


-0.8 


179.522 


-41.5 


1 . 334 


+2.6 


207.464 


+29.6 


5.010 


+2.0 


225.499 


+ 18.8 


4.846 


+0.3 


417.853 


-50.7 


3.078 


-1.6 


424.868 


-20.9 


4.027 


+0.1 


425.852 


+29.5 


5.011 


+ 1.9 


438.778 


+52.2 


5.804 


-2.7 


449.706 


+5.8 


4 . 599 


+0.5 


453.851 


-50.4 


2.678 


+5.1 


455.837 


+8.5 


4.664 


-0.2 


456.837 


+60.3 


5.664 


+5.7 


459.856 


-52.3 


2.617 


+3.8 


460.737 


-36.1 


3.498 


+2.8 


462.756 


+49.2 


5.517 


-2.2 


464.724 


-45.2 


1.418 


+ 1.8 


467.760 


-1.7 


4.454 


+0.3 


469.703 


+24.1 


0.331 


+0.8 


472.708 


-44.8 


3.336 


-1.5 


476.803 


-44.4 


1.365 


+0.8 



The following observations were not used to obtain 
the final solution. 
099.814 +8.1 

166.604 +13.8 

4.57.808 +18.8 





TABLE IV 
Orbital Elements of 


AR Cas 


Element 


Preliminary 


Final 


P (days 
T (J.D.) 

n 

e 

K (km /sec) 
7 _ (km /sec) 
a sin i (lO^km) 
f(m) O 


6.0663309 
2440087.219 
30 
0.22 

.56.5 
-10.3 


6.066.3309 
2440087.193 ±0.013 
31.4 ±0.8 

0.245 ±0.012 
56.7 ±0.7 
-13.4 ±0.5 
4.. 59 ±0.06 
0.095 ±0.004 



104 



Walter L. Gorza cmd John F. Heard 



and the adopted velocity curve. The error of a single observation was 
found to be ±2.8 km/sec. 

It can be seen that the value for co here obtained (that is, u = 31°4) 
and the identical result obtained by Petrie in 1958 (Batten, 1968), 
together with the two photoelectric solutions by Stebbins (co = 37°2o) , 
and by Huffer and Collins (oj = 3-4°± 5°), seem to rule out the sug- 
gestion that there is a rotation in the line of apsides. If, nonetheless, 
small variations in the value of co are real, then, the suggestion by 
Batten (1960, 1961) that a third body may be present in the system 
would explain these variations and the variations that Batten found 
in the value of \'o, the systemic velocity. 











• These points were not used in the 
solution. 


60 


- 






o 


40 


\ 


AR Cos 




/a \ 


20 


« • 






/ » * 


Vo 

(km/tecj 



\« 






/ \* 


-20 








\ 


-40 




^^eS>o. °£^ 


0/ 


^*-><^ 


-€0 


. 


o 

1 1 


1 


1 1 1 I 



0-0 



10 



20 



50 40 &0 

Phase (days) 



eo 



70 



ao 



Fig. 2 — Velocity Curve for the Eclipsing Binary .^R Cas. 



H.D. 11636 (pAri) 

The first spectroscopic orbital solution to this star (awoo = OP 49™ 1, 
5 = +20° 19', niptg = 2.86, Sp. = Ao) was obtained by Ludendorff 
(1907), and another by Petrie (1938). Because of the unusually large 
orbital eccentricity, Dommanget suggested that this ma}' be an 
excellent system in which to observe the "periastron efTect". 

Following receipt of a list of binary stars in need of spectroscopic 
observation from Commissions 30 and 42 of the I.A.U., the star was 



spectroscopic Orbits of Four Binary Systems 



10.5 



placed on our observing program and 44 plates were obtained between 
August 31, 1968 and June 11, 1970. (On two occasions three plates 
were obtained very close together in time and were combined into 
normal places.) Since the period of the system is so very close to an 
integral number of da\-s, no observations can be made at the present 
time, of the maximum point in the velocity curve from observatories 
in North America. This point now crosses the meridian during daylight, 
and it will be the end of the centur>- before it will again cross the 
meridian at a time when observations can be made, as it was at the time 
of Petrie's observations. For this reason our preliminary elements 
were obtained with the help of some of Petrie's observations near the 
maximum point of the velocity curve. The least-squares differential 
correction, however, was carried out only on our own observations. 
The value for the period (as given by Petrie) was held constant. The 
observations are listed in Table \\ while Table \l gives the preliminary 
and the final elements. Figure 3 shows the individual observations and 
the adopted velocity curve. The error of a single observation was found 
to be ±2.3 km/sec. 




50 60 70 
PtiQse (days) 



Fig. .3 — \'elocit\- Curve for the Spectroscopic Binary ^ Ari. 

The value for w ol)tained by Ludendorff is 21?88. that l)y Petrie 
24?17 and the present one 20?01. Leaving aside Ludeiidorff's solution 
(only two lines at the most could be measured on each plate), and if the 



lOG Walter L. Gorza and John F. Heard 

TABLE V 
Radial-Velocity Observations of ^ Ari 



J.D. 


\'o 


Phase from 


0-C 




2440000+ 


km /sec 


Final T 


km /sec 




99.789 


+27.6 


105.385 


-2.2 




106.844 


-10.6 


5.443 


-3.1 




120.807 


-4.S 


19.406 


+5.0 




143.692 


-3.4 


42.291 


+5.1 




151.698 


-8.6 


50.297 


-0.7 




158.723 


-7.0 


57.322 


+0.2 




199.574 


+2.3 


98.173 


-1.6 




207.451 


+45.1 


106.050 


+2.5 




223.038 


-9.4 


14.639 


+0.4 




258.499 


-7.1 


50.100 


+0.8 




417.863 


+8.0 


102.467 


-3.3 




421.856 


+54.6 


106.460 


-0.6 




425.867 


-6.9 


3.474 


-2.3 




432.840 


-9.3 


10.447 


+0.2 




436.889 


-12,1 


14.496 


-2.3 




438.790 


-10.5 


16.397 


-0.7 




438.890 


-13.3 


16.497 


-3.5 




453.866 


-9.7 


31.473 


-0.4 




455 . 849 


-10.6 


33 . 456 


-1.4 




456.877 


-9.5 


34 . 484 


-0.4 




457.818 


-12.2 


35.425 


-3.2 




459.867 


-9.2 


37.474 


-0.3 




460.831 


-10.4 


38.438 


-1.6 




462.871 


-10.9 


40.478 


-2.2 




464.744 


-6.5 


42.351 


+2.0 




467 . 872 


-9.5 


45 . 479 


-1.2 




469 . 724 


-7.3 


47.331 


+0.8 




472.763 


-7.2 


50.370 


+0.7 




476.813 


-6.5 


54.420 


+ 1.0 




477.832 


-7.9 


55 . 439 


-0.5 




478.863 


-5.6 


56.470 


+ 1.7 




479.862 


-6.5 


57.469 


+0.7 




486.817 


-6.1 


64.424 


+0.4 




503.633 


-6.3 


81.240 


-2.5 




510.672 


+ 1.5 


88.279 


+3.4 




733.855 


+7.1 


97.467 


+3.9 




743.839 


+37.4 


0.454 


0.0 




744.839 


+6.4 


1.454 


-0.9 




745.849 


+3.7 


2.464 


+4.8 




746.851 


-3.5 


3.466 


+ 1.1 






TABLE 


VI 






Orbital Elements of /3 Ari 






Element 


Preliminary 




Final 




P (days) 


106.9973 




106.9973 


T (I.D.) 


2440208.286 


2440208.398 


±0.033 


w (°j 


25 . 5 




20.0 


±1.3 


e 


0.89 




0.896 


±0.003 


K (km/sec) 


38.1 




37.1 


±0.9 


7 (km /sec) 


-3.8 




-4.0 


±0.4 


a sin i (10«km) 






24.3 


±0.7 


f(m) O 






0.050 


±0.004 



i 



spectroscopic Orbits of Four Binary Systems 107 

criterion is used that only variations that exceed three times their 
probable error are real (Batten, 1968) then, since the mean error is 
±1°28 (i.e. a probable error of ±0°86), it would appear that the varia- 
tion in the value of w — 41°6 in 82 years — though small, may be real. 

H.D. 209813 

Four plates of this star (a = 22>^01'"0,5 = +4()°45',m,. = G.;y2, Sp. = 
KO III) taken at this Observatory in 193.5-37 showed it to be a spec- 
troscopic binary, and from 39 plates taken in 194.5-46 the late Miss 
Ruth Xorthcott (1947) computed an orbit using a period of 24.431 days 
derived with the help of the first four plates. The 1945-46 plates were 
from the prism spectrograph with dispersion of 33 A/mm. On six of iier 
plates which were strong in the violet region Aliss Northcott was able 
to see H and K lines in emission and to measure the velocities; they 
appeared to follow the velocities from the absorption lines. 

Blanco and Catalano (1968) observed a slight variability of the light 
of H.D. 209813 to which they at first assigned a period of 25.98 days. 
Not being aware that the star had been studied as a spectroscopic 
binary, they suggested that the star was probably a Cepheid variable. 
Fernie, Hube and Schmidt (1968) of this Observatory replied that 
there were reasons to doubt the Cepheid explanation, and that the 
light variations should be re-examined relative to Miss Northcott's 
period to see if an explanation could be found in terms of an eclipsing 
system. At the same time we put the star on our spectroscopic ob- 
serving program for a second orbit determination. 

From a combination of our 30 1968-70 observations (which are 
listed in Table VII) and Miss Northcott's 1945-46 observations we 
have improved the period to 24.4284 days. We then solved for the 
remaining elements wliich are shown in Table \'III. Also in this table 
are listed the results of a new solution for Miss Northcott's ol^serva- 
tions which uses tlie improved period. Figure 4 shows our oljservations 
and the velocity curve representing our elements. 

A comparison of the new elements from the 1945-46 observations 
and tlie elements from the 1968 70 observations calls for the following 
conuuents. In view of the smallness of the eccentricity' tlie difterences 
in the values of e and oo are not regarded as necessarih' significant. The 
difference in 7, the systemic velocity, finds an easy explanation in the 
fact that different spectrographs were used, llie difference of 1.5 
km/sec in the value of K, the semi-amplitude, may be significant; it 
is about three times the mean error of either determination, and on a 
plot of tlie two sets of ol)servations it was (juite apparent. If it is indeed 
real it is teni])ting to tliink of an exjilanation in terms of mass transler 



108 



Walter L. Gorzn and John F. Heard 



TABLE VII 
Radial \'elocities and H and K Emission Widths 







Phase from 








J.D. 


Vabs 


Final T 


0-C 




Em. Width 


2400000+ 


km /sec 


Days 


km /sec 


V em 


km /sec 


39999.974 


-60.1 


7.231 


-3.1 


_ 




40099.719 


-47.6 


9.263 


+0.4 


-48.4 


68 


40100.786 


-41.4 


10.330 


-0.9 


-49.7 




40103.663 


-16.2 


13.207 


-0.5 


-14.4 


70 


40104.630 


-7,6 


14.174 


0.0 


-8.5 


63 


40107.835 


+ 10.2 


17.379 


+0.4 


+ 10.1 


60 


40112.717 


-2.6 


22.260 


+ 1.9 


0.0 


67 


40120.651 


-57.8 


5.766 


+0.2 


-60.7 


59 


40125.773 


-36.8 


10.888 


-0.8 


— 


— 


40133.664 


+ 13.1 


18.779 


+2.2 


+ 10.9 


61 


40140.688 


-32.4 


1.375 


+2.3 


-36.2 


67 


40143.588 


-56.2 


4 . 275 


— 2.2 


-58.7 


— 


40151.647 


-23.6 


12.334 


-0/2 


-23.5 


62 


40161.647 


-2.4 


22.334 


+2.7 


-6.4 


66 


40179.579 


+3.1 


15.838 


-0.6 


+0.8 


64 


40424.809 


+6.8 


16.784 


-1.2 


+6.2 


62 


40459.784 


-49.2 


2.902 


-2.8 


-46.2 


65 


40486.762 


-57.1 


5.451 


+0.5 


-58.1 


__ 


40779.822 


-55.6 


5.370 


+ 1.8 


-63.4 


— 


4()7it4.653 


+8.2 


20.211 


+0.7 


+ 14.0 


— 


4()SO().783 


-39.4 


1.903 


-0.3 


-40.9 


68 


4()S(I4.799 


-57.0 


5.919 


+ 1.1 


-57.7 


75 


4()S2().774 


-5.8 


21.894 


-3.9 


+3.6 


57 


40866.724 


+9.2 


18.987 


-1.5 


+ 13.1 


— 


40869.513 


-0.7 


21.776 


+0.4 


+9.6 


69 


40878.644 


-57.1 


6.479 


+ 1.0 


-54.0 


64 


40879.692 


-55.2 


7.527 


+ 1.0 


-57.5 


68 


40883 . 679 


-27.8 


11.514 


+2.8 


-31.3 


57 


40895.481 


-13.4 


23.315 


-0.4 


-11.2 


73 


40896.600 


-23.4 


0.007 


-0.6 


-20.5 


70 



TABLE VIII 
Orbital Elements of H.D. 209813 



Element 


Preliminary 


Final 


Xorthcott's (re- 


computed) 


P (davs) 


24-: 4284 


24. 4284 ± 0.0005 


24.4284 


± 0.0005 


T (J.D.) 




2440017.170 ± 0.054 


J.D. 2431661.692 


± 0.070 


« (°) 





89 ±15 


73 


± 6 


e 





0.009 ± 0.003 


0.026 


± 0.003 


K (km/sec) 


35.3 


34.6 ± 0.4 


33.1 


± 0.6 


7 (km/sec) 


-24.2 


-23.6 ± 0.3 


-22.2 


± 0.4 


a sin i (lO^km) 




11.6 ± 0.2 


11.1 


± 0.2 


f(m) O 




0.105 ± 0.005 


0.092 


± 0.005 



The mean error of the period is estimated. 



spectroscopic Orbits of Four Binary Systems 



109 



10 

Vo 

(km/sec) 


- 


H.D. 209813 




/o 


o 


o\ 






-10 


■ 




J 












-20 


1 




1 








\ 




-30 


\ 




o/ 








\ 




-40 


i \ 


V 


/ 








^ 


V 


-50 




o\ / 














-60 




o 
1 










1 





5 10 15 20 25 30 

Phase(days) 

Fig. 4 — \'elocity Curve for the Spectroscopic Binary H.D. 209813. 

Ijetween the components. Althougli it is difficult to l^elive that stifficient 
mass could be transferred in 24 years to affect the mass ratio by an 
observable amount, it may be that the elements are affected by a 
process of gas streaming which for this star changes its pattern with 
time. The idea that motion of this star's atmosphere plays a role in the 
measured radial velocities is suggested by the fact that a few of our 
residuals (0-C in Table \TI) are larger than 2.5 km/sec. Such large 
residuals we have never encountered in our measures of spectrograms 
of standard-velocity stars with the 12 A/mm spectrograph. Also the 
mean error of a single observation for H.D. 209813 is dzl.6 km/sec 
compared with ±1.1 km/sec for measures of standard-velocity stars. 
We have been able to study the Ca II emission lines better than 
could Miss Northcott from her prism spectrograms. The velocities 
which we obtained from measures of H and K emission lines are listed 
in Table VII; the overall mean value of Vabs — \ em is —0.2 km/sec. 
Also we have measured the widths of the emission lines, the mean 
widths being listed in Table VII. The overall mean width is 65 km/sec. 
This gives for the star an absolute magnitude of My = -fO.8 according 
to the correlation of Wilson and Bappu (1957). Neither the widths nor 
the differences between the H- and K- and the absorption-line velocities 
seem to correlate \\'\\\\ the orbital period or any period near 24 da>'s, 



110 Walter L. Gorzn und John F. Heard 

and, in fact, we believe that the widths are constant and that the 
velocity differences between emission and absorption lines are zero. 

To return to the question of the light variability of H.D. 209813, 
Blanco and Catalano (1970) in the light of new observations have 
revised their period from 25.98 days to 25.3 days, but they state that 
their photometric observations are not at all satisfied by the orl)ital 
period, and that there are changes in the light curves of 1967 and 1968 
and also apparent Huctuations in the period. For these and other 
reasons they reject the suggestion that the light variations are associ- 
ated with eclipses. 

A model to explain tlie light variability and its period remains to be 

TABLE IX 
List of Wave-Lengths used in the Determination of the Radial Velocity for: 



H.D. 128661 


AR Cas 




/ 


3 Ari 




H.D 


. 209813 


Fe I 3820.428 


H16 


3703 


855 


H16 


3703 


855 


Mn I 


4034.490 


Fe I 3825.884 


H15 


3711 


973 


H15 


3711 


973 


Mn I 


4035.728 


Fe I 3859.913 


H14 


3721 


940 


H14 


3721 


940 


Mn I 


4041.361 


Fe I 3865.. 526 


H13 


3743 


370 


H13 


3734 


370 


Mn I 


4055 . 543 


Fe I 3920 . 260 


H12 


3750 


1.54 


H12 


3750 


1.54 


Gd II 


4078.444 


Fe I 3922.914 


Hll 


3770 


632 


Hll 


3770 


632 


Fe I 


4156.803 


Fe I 3927.922 


HIO 


3797 


900 


HIO 


3797 


900 


Fe I 


4174.917 


Fe I 3930.299 


He I 


3819 


606 


Fe I 


3820.428 


Fe I 


4187.044 


Ca II 3933.664 


H9 


3835 


386 


H9 


3835 


386 


Co I 


4190.712 


All 3944.009 


H8 


3889 


051 


Si II 


3856 


021 


Fe I 


4199.970 


Sr 11 4077.714 


He 


3970 


075 


H8 


3889 


051 


Fe I 


4202.031 


Si II 4130.876 


He 1 


400!) 


270 


Ca II 


3933 


664 


Fe I 


4210.352 


Fe I 4181.7.58 


He I 


4026 


140 


Sr II 


4077 


714 


Fe I 


4219.364 


Fe I 4202.031 


H5 


4101 


738 


H6 


4101 


738 


Fe I 


4233.608 


Sr II 42 15. 524 


He 1 


4143 


7.59 


Sr 11 


4215 


524 


Fe I 


4238.816 


Fe I 42.50.125 


Hy 


4340 


466 


H7 


4340 


466 


Fe I 


4239.847 


Fe I 4271.764 


He I 


4387 


928 


M^ II 4481 


228 


Fe I 


4245.258 


Fe I 4.383.. 547 


He I 


4471 


477 


S II 


4549 


550 


Fe I 


4271.764 


Fe I 4404 . 7.52 


H^ 


4861 


332 


H^ 


4861 


332 


Fe I 


4325.765 


Ti II 4468.493 














Cr I 


43.59.631 


Ti II 4.501.449 














Fe I 


4375.932 


Fe II 4.508.283 














Fe I 


4383.547 


Fe II 4515.337 














Fe I 


4389.244 


Ba 11 4.")."i4.926 














Gd II 


4390.953 


Ti II 4571.971 














Fel 


4442 . 343 


Fe 11 4.583.829 














Fe I 


4447.722 


Fe 1 1 4629 . 323 














Fe I 
Fe I 
Fe I 
\- I 
Cr I 
Cr I 
Fe I 
Col 
Ba II 
Cr I 
Fe I 
Fe I 


44.59.121 
4466 . 554 
4476.021 
4496.864 
4.526.466 
4.527.339 
4.528.619 
4.533.985 
45.54.033 
4565.512 
4602.944 
4934.023 



spectroscopic Orbits of Four Binary Systems 1 1 1 

found. Probal)l\' a discussion in terms of gas streaming witliin tlie 
geometry of the Lagrangian surfaces would be illuminating in this 
regard. Meanwhile it seems clear that H.D. 209813 belongs to a group 
of spectroscopic binaries which all show greath- enhanced H and K 
emission (Hiltner 1947; Gratton 1950; Abt, Dukes, and Weaver 1969). 
Whether or not these other s\'stems show light variability of the type 
seen in H.D. 209813 is important in determining a general model for 
their behaviour, and such an investigation is currently being carried 
out b\" Air. William llerbst at this Observatory. 

Ackn owl edge tn 02 fs 

The writers were assisted b\' a grant from the National Research 
Council (J.F.H.) and by an Ontario Graduate Fellowship and a Uni- 
versity of Toronto Summer Scholarship (W.L.(i.). We are indebted 
to Dr. A. H. Batten of the Dominion Astroplu'sical Observatory 
for valuable discussion regarding AR Cas and f3 Ari, and to Dr. J. D. 
Fernie relative to H.D. 209813. 

Referenxes 

Abt, H. A., Dukes, R. J. and Weaver, \V. B. 1969, Ap. J., 157, 717. 
Baker, R. H. 1910, Allegheny Obs. Pub., 2, 28. 
Batten, A. H. 1960, P.A.S.P., 72, ;349. 

, 1961, J.R.A.S. Canada, 55, 120. 

, 1968, J.R.A.S. Canada, 62, ;344. 

■ , 1968, Pub. Dom. Astrophys. Obs. Victoria, 13, 119. 

Blanco, C. and Catalano, S. 1968, I.A.U. Inf. Bull. Var. Stars, no. 2.53. 

, 1970, Astr. and Astrophys., 4, 482. 

Fernie, J. D., Hube, J. O. and Schmidt, J. L. 1968. I.A.U. Inf. Bull. Var. Stars, no. 

263. 
Frost, E. B. and Adams, \V. S. 1903, Ap. J., 18, 383. 
Gratton, L. 19.50, A p. J., Ill, 31. 

Harris, A. J. 1969. I.A.L'. Inf. Bull. Var. .Stars, no. .36."). 
Hiltner, \V. A. 1947, A p. J., 106, 481. 

Huffer, C. M. and Collin--, G. W". 1962, Ap. J. SuppL, 7, 3.51. 
Jackisch, G. 1968, I.A.U. Inf. Bull. Var. Stars, no. 314. 
Lehmann-Filhes, R. 1894, A. X., 136, 17. 
Ludendorff, H. 1907, A p. J., 25, 320. 

Luyten, \V. J., Struve, O. and Morgan. W". \V. 1939, Verkes Obs. Pub., 7, 281. 
Xorthcott, Ruth J. 1947, David Dunlap Obs. Pub., I, no. 19. 
Petrie, R. M. 1938, Pub. Dom Astrophys. Obs. Victoria. 7, 10.5. 

, 1944, .4. J., 51, 22. 

Petrie, R. M. 1962, Stars and Stellar Systems, ed. \\". A. Hiltner (Chicago and London: 

The University of Chicago Press) 2, ch. 23. 
Stebbins, J. 1921, A p. J., 54, 81. 
.Sterne, T. E. 1941, Proc. Nat. Acad. Sci., 27, 175. 
Wilson, O. C. and Bappu, M. K. \'. 19.57, 1/;. J.. 125, (iOl. 



PUBLICATIONS OF 

THE DAVID DUNLAP OBSERVATORY 

UNIVERSITY OF TORONTO 

Volume 3 Number 5 



THE ESTABLISHMENT OF 21 NEW 

NINTH MAGNITUDE lAU STANDARD 

RADIAL VELOCITY STARS 



JOHN F. HEARD 

AND 

CH. FEHRENBACH 



1972 
TORONTO, CANADA 



PUBLICATIONS OF 

THE DAVID DUNLAP OBSERVATORY 

UNIVERSITY OF TORONTO 

Volume 3 number 5 



THE ESTABLISHMENT OF 21 NEW 

NINTH MAGNITUDE lAU STANDARD 

RADIAL VELOCITY STARS 



JOHN F. HEARD 

AND 

CH. FEHRENBACH 



1972 
TORONTO, CANADA 



PRINTED AT 
THE UNIVERSITY OF TORONTO PRESS 



THE ESTABLISHMENT OF 21 NEW NINTH MAGNITUDE 
lAU STANDARD RADIAL VELOCITY STARS 

By John F. Heard, David Dunlap Observatory 
and Ch. Fehrenbach, Observatoire de Haute Provence 

ABSTRACT 

Twenty-four stars of photographic magnitude 8.26 to 9.64 and of spectral 
types F, G and K, in the decUnation zone +25° to +30° have been investigated 
for suitability as an extension of the lAU hsts of standard velocity stars. The 
stars were observed with dispersions of 12, 20 and 15 A/mm at the David 
Dunlap, Haute Provence and Dominion Astrophysical Observatories respec- 
tively, and the spectrograms were measured with systems tested against the 
lAU system. Three of the 24 stars are believed to have small-range velocity 
variations. The remaining 21 are presented as new lAU standard velocity 
stars. 

INTRODUCTION 

At lAU Symposium no. 30 on "Determination of Radial Velocities and 
their Application" (Batten and Heard 1967), Fehrenback drew attention to 
the need for an extension of the lists of lAU. standard velocity stars to include 
stars which are appreciably fainter than those in Table 2 of the Report of 
Sub-commission 30a in the Transactions of the International Astronomical 
Union, volIX, 1955. 

In 1967 Heard reported to the lAU Commission 30 meeting in Prague the 
selection of 24 stars in the declination zone +25° to+30°Vkath spectral types 
ranging from F7 to K5 and photographic magnitudes 8.26 to 9.64 which had 
already appeared to have constant velocities (Heard, 1956). He proposed to 
re-observe these stars at higher dispersion at the David Dunlap Observatory 
and invited participation by others. 

OBSERVATIONS 

Observations of the 24 stars were begun at the David Dunlap Observatory 
in 1968 and continued through 1971. The 12 A/mm dispersion of the Casse- 
grain grating spectrograph was used with the 188-cm telescope, and the goal 
was to obtain seven spectrograms of each star. 

At rObservatoire de Haute Provence Fehrenbach also undertook observa- 
tions of these stars with the 20 A/mm dispersion of the coude spectrograph of 
the 152-cm telescope, and in 1970 and 1971 obtained from three to five 
spectrograms of most of the stars. 

Through the kindness of Dr. K.O. Wright and his colleagues, a total of 22 
spectrograms of the stars were also obtained at the Dominion Astrophysical 
Observatory with the 15 A/mm dispersion of the Cassegrain grating spectro- 
graph of the 183-cm telescope. 

The results which follow are based on these three sets of observations 
which include a total of 277 spectrograms of the program stars. In addition. 



113 



1 14 John F. Heard and Ch. Fehrenbach 

133 spectrograms of existing lAU standard velocities stars were measured to 
ensure that the new velocities conform to the lAU system. 

After reporting our preliminary results at the meeting of lAU Commission 
30 in 1970, we were authorized to present the final results as lAU standards. 

MEASUREMENT AND REDUCTION 

David Dunlap 

The Dunlap plates were measured on a Jenna Abbe comparator, four 
settings being made on both iron arc comparison lines and star lines in each 
direction of traverse. The star lines were a selection (usually between 20 and 
28 in number) of the wavelengths listed by Gorza and Heard (1971). The 
reductions were made either by the usual method of tables of standard set- 
tings and correction curves or by a computer program which effectively estab- 
lishes the dispersion curve of each spectrogram. We compared the two 
methods and found that the difference seldom exceeded 0.1 km/sec. 

Although our lists of lines had been, in the first place, selected with care as 
a result of measurements of lAU standard velocity spectrograms, we feared 
that the special conditions of observation of the faint program stars (pro- 
jected slit width 33//, projected slit length 0.3 mm, long exposures and some- 
times large hour angles) miglit introduce systematic errors. In an effort to 
determine such errors if they existed, we observed lAU standard velocity stars 
almost nightly under conditions similar to those for the program stars, at- 
tempting to match the quality of the spectrograms. Fifty-six such standard 
velocity spectrograms were measured and reduced. Tlie results are summarized 
in Table 1 which lists, for F-,G-and K-type spectra separately, the residuals in 
the sense lAU-DDO and the average corrections which are apphcable to our 
velocities to bring them to the lAU system. Although the mean errors of 
these corrections reveal them to be only marginally significant, we did never- 
theless apply these small corrections to the Dunlap program star velocities. 

A study of the standard velocity results failed to reveal any correlations of 
residuals with length of exposure, hour angle, plate density or seeing. 

Dominion Astrophysical 

Of the 22 available DAO 15 A/mm spectrograms of the program stars, 11 
were taken with the spectrograph fitted with a conventional slit and the 
remaining 1 1 with the use of a Richardson image-slicer. Because these plates 
became available to us before a standard system of selected wavelengths had 
been made by the DAO astronomers, we used the wavelengths which had 
been selected for the DDO 12 A/mm spectrograms, and, to determine the 
systematic corrections which might thus be introduced, we measured six 
spectrograms of each of F-, G- and K-type standard velocity stars taken with 
the conventional slit. The results for the 18 spectrograms gave an average 
residual (lAU-DAO) of -0.8 ±0.3. This agrees well with the findings of 
Aikman (1971) who got a residual of about this same amount for DAO 



21 New 9 th Magnitude I A U Standard Radial Velocity Stars 1 1 5 

standard velocity spectrograms, measuring them in a different manner with a 
different wavelength selection. The samples used by both us and Aikman 
were too small to give a significant break-down of the residuals by spectral 
class. Accordingly, we corrected the measured velocities of all 11 of the 
conventional-slit spectrograms of program stars by -0.8 km/sec. 

Aikman also reported a test of image-slicer standard velocity spec-trograms 
and found no statistically significant mean residual for them. We tested our 
measures of the image-slicer program star spectrograms by re-computing the 
velocities according to the wavelengths used by Aikman and found the mean 
residual to be only 0.1 km/sec. Accordingly, we made no corrections to our 
measured velocities for these image-slicer spectrograms. 

Haute Provence 

The methods of measurement and reduction of the Haute Provence 20 
A/ mm spectrograms have been described by Fehrenbach (1972) who also 
analysed the results from 59 spectrograms of lAU standard velocity stars. 
Because he found the residuals, lAU-OHP, to be small and statistically insig- 
nificant, we have applied no corrections to the Haute Provence velocities of 
the program stars. 

RESULTS 

The results for the 24 program stars are summarized in Table II. 

Column 1 gives the designation and (for the three stars not listed in Table 
III as new standards) the 1950 co-ordinates, the photographic magnitude and 
the spectral classification, the last two data being quoted from the results of 
Heard (1956). 

Columns 2, 5, 8 give the Julian dates of the observations. Columns 3, 6, 9 
give the velocities (corrected to the lAU system as indicated earlier), and 
columns 4, 7, 10 give the internal mean errors, i.e. 



/ S V 
Ci = 



n(n-l) 



where n is the number of lines measured and v is the deviation of the velocity 
of a line from the mean velocity for the plate. 

Below the plate velocity entries in columns 2, 5, 8 are given the mean 
velocities from each observatory followed by the external mean errors, i.e. 



£.= M^ 



N(N-l) 



where N is the number of spectrograms and V is the deviation of the velocity 
of a plate from the mean velocity for the N plates. 



116 John F. Heard and Ch. Fehrenbach 

Tliree stars, namely BD + 29° 1553, HD 160952 and HD 204934 show 
sufficient evidence of small-range variation of velocity to warrant their exclu- 
sion from the list recommended as new standards of velocity. 

The new list of 21 lAU standard velocity stars is given in Tahle III. 

Finally, we have the following comments on the results which we believe 
support their validity: 

Our observations having been carried out over at least two years and more 
often three, there seems to be little chance that long-period variations have 
been missed. 

For the determinations at the three observatories considered separately, 
the average values of the external mean errors per star are DDO ± 0.5, OHP 
± 0.5, DAO ± 0.7, whereas the average values of the residuals between ob- 
servatories are DDO-OIIP = -0.2, DDO-DAO = +0.2. These residuals, then, 
seem not to be statistically significant. 

Comparing the average external mean error per star in the list of lAU 
standard velocity stars fainter than magnitude 4.3 as given in lAU Transac- 
tions vol. iX p. 443 (after converting Iroin V.\L. to M.E.) with ours, we find 
that ours is somewhat better (0.34 compared to 0.44) in spite of the fact that 
the average number of observations per star is greater in the lAU list than in 
ours. 

ACKNOWLEDGEMENTS 

We gratefully acknowledge the help of colleagues at the three observatories 
in the obtaining of the spectrograms, and we thank Mr. Mark McCutcheon 
and Miss Molly Morrow at the David Dunlap Observatory and Mr. and Mrs. H. 
Petit at the Haute Provence Observatory for the measuring of most of the 
plates. One of us (J. F.I I.) has received support for the project in the form of a 
research grant trom the National Research Council of Canada. 



REFERENCES 

Aikman, C.L. I^>7I , private communication. 

Batten, A. II. and Heard, .I.F. V)bl , Dc terminal itm of Radial Velocities and 

their Applications (London: Academic Press), p. 70. 
I'ehrciibach, Ch. 1972, /l.v/r and Astrophys. (in press). 
Gor/a, W.L. and Heard, J.F. 1971 , David Dunlap Ohs. Pid).. 3, 99. 
Heard, J.F. 1956, David Dunlap Ohs. Pub., 2, 107. 



21 New 9 th Magtiitude I A U Standard Radial Velocity Stars 1 1 7 



TABLE I 





RADIAL VELOCITY RESIDUALS FROM lAU STANDARDS 








MEASURED ON DUNLAP SPECTROGRAMS 






F-type 


G-type 


K-type 


HD 


Sp. 


lAU-DDO 

km/sec 


HD 


Sp. 


lAU-DDO 

km /sec 


HD 


Sp. 


lAU-DDO 

km/sec 


22484 


F8 V 


+0.3 


65583 


G8 V 


-1.6 


3712 


KOII-III +1.1 






+0.9 




















84441 


GO 11 


+1.5 


3765 


K2 V 


+1.1 


36673 


FOIb 


+1.3 




















103095 


G8 V 


+0.9 


9138 


K4 1II 


+1.3 


89449 


F6IV 


+1.2 
-2.0 






-0.9 






+0.1 
+1.4 






+0.7 


109379 


G5 III 


+0.5 






+1.6 






-0.1 






-0.4 






+1.8 






+0.1 


171391 


G8III 


-0.5 






+0.6 
+0.6 


102870 


F8 V 


+0.2 






-1.4 






-0.6 


136202 


F8IV 


+0.3 
+0.3 


204867 


GO lb 


+0.3 
+0.3 
+1.5 


26162 
29139 


gKl 
K5 III 


+0.7 
-1.8 


187691 


F8 V 


+0.8 






-0.6 
-0.6 






+1.3 


222368 


F7 V 


+0.6 






+1.5 
+0.4 


35410 
66141 

92588 
107328 
186791 
212943 


KOIII 
K2III 

Kl IV 
KOIII 
K3II 
KOIII 


0.0 
0.0 

+1.6 

+1^ 
-2.0 
-1.7 
-0.2 
-1.7 
-0.4 

-1.5 

-0.8 

+1.5 

-0.1 
+0.7 


1 3 plates 


mean +0.3 ±0.2 


15 plates, mean 0.0 ±0.1 


28 plates 


, mean - 


-0.2±0.2 



118 



John F. Heard and Ch. Fehrenbach 



TABLE II 
RADIAL VELOCITY MEASURES OF THE PROGRAM STARS 



STAR 


DAVID DUNLAP 


HAUTE PROVENCE DOMINION ASTROPHYSICAL 




J.D. 


Vel. 




J.D. 


Vel. 


J.D. Vel. 




244. . . km /sec 


£ 1 


244. . . km/sec 


^ * 244. . . km/sec ^ ^ 


HD4388 


0525.7 


-30.0 


0.6 


0856.5 


-29.5 


0.5 




0532.6 


-28.4 


0.5 


0858.5 


-27.0 


0.7 




0571.6 


-32.2 


0.6 


0862.5 


-25.9 


0.5 




0784.2 


-27.3 


0.6 










0793.2 


-26.2 


0.6 










0834.7 


-28.0 


0.5 










0849.8 


-28.7 


0.4 












-28.7 


±0.7 




-27.5 


±1.0 


HD 12029 


0578.6 


+37.1 


0.8 


0850.5 


+37.8 


0.5 0480.0 +39.1 0.6 




0804.8 


+38.3 


0.6 


0851.6 


+38.1 


0.6 




0806.9 


+38.1 


0.2 


0853.5 


+43.7 


0.5 




0834.8 


+37.4 


0.3 


0873.0 


+36.8 


0.5 




0875.5 


+39.7 


0.5 


0874.6 


+38.1 


0.6 




0923.5 


+39.6 


0.4 












+38.5 


±0.4 




+38.9 


±1.2 +39.1 


HD 14969 


0621.5 


-32.6 


0.4 


0852.6 


-33.0 


0.7 




0849.8 


-35.2 


0.5 


0862.6 


-32.6 


0.5 




0895.7 


-32.6 


0.8 


0866.5 


-33.2 


0.9 




0951.5 


-34.9 


0.3 


0873.6 


-32.5 


0.8 




0953.5 


-32.5 


0.4 










0958.5 


-34.9 


0.5 












-33.8 


±0.6 




-32.8 


±0.2 


HD 23169 


0578.7 


+12.9 


0.9 


0858.6 


+14.2 


0.5 




0594.7 


+12.6 


0.8 


0872.6 


+14.0 


0.5 




0624.6 


+13.2 


0.7 


0873.5 


+14.8 


0.3 




0640.6 


+13.5 


0.8 


0874.5 


+13.3 


0.5 




0927.8 


+13.0 


0.9 


0892.6 


+12.8 


0.4 




0951.5 


+11.9 


0.7 










0953.5 


+ 13.0 


0.5 










0993.5 


+14.2 


0.6 












+ 13.0 


±0.3 




+ 13.8 


±0.4 


HD 32963 


0223.7 


-64.0 


0.8 


0855.6 


-60.0 


0.6 




0259.5 


-62.2 


0.6 


0857.6 


-64.0 


0.6 




0266.5 


-63.4 


0.6 


0866.5 


-64.5 


0.4 




0624.7 


-63.7 


0.5 


0872.6 


-63.7 


0.4 




0849.9 


-64.2 


0.4 


0874.6 


-62.4 


0.6 




0941.8 


-63.4 


0.6 


1190.6 


-60.8 


0.4 




0942.7 


-64.1 


0.7 









-63.6 ±0.3 



-62.6 ±0.7 



21 New 9 th Magnitude I A U Standard Radial Velocity Stars 1 1 9 

TABLE U-continued 



STAR 


DAVID DUNLAP 


HAUTE PROVENCE DOMINION ASTROPHYSICAL 




J.D. 


Vel. 




J.D. 


Vel, 




J.D. 


Vel. 






244. . . 1 


km/sec 


S 1 


244. . . 


km/sec 


£ 1 


244. . . 


km/sec 


e 1 


HD 42397 


0259.6 


+38.1 


0.4 


0872.6 


+36.5 


0.5 


1026.7 


+35.3 


0.6 




0270.7 


+36.2 


0.5 


0873.7 


+37.0 


0.4 










0280.6 


+40.5 


0.6 


0892.7 


+39.4 


0.5 










0660.6 


+36.9 


0.7 


0893.6 


+36.9 


0.5 










1001,5 


+37.3 


0.8 
















1015.5 


+37.6 


0.6 
















1020.5 


+37.0 


0.7 


















+37.7 


±0.5 




+37.5 


±0.7 




+35.3 




BD+29°1553 


0259.7 


-7.8 


0.6 














07'^31."i4 


0657.6 


+ 1.2 


0.9 














+28051' 


0665.6 


+0.5 


0.6 














9.29 


0675.6 


-2.0 


0.7 














GO IV 


0681.6 
0951.8 


-1.8 

-5.4 

Var. 


0.9 
0.6 














HD 65934 


0207.8 


+34.7 


0.3 


1051.3 


+36.5 


1.3 










0280.7 


+35.4 


0.3 


1052.3 


+35.1 


0.8 










0595.8 


+34.8 


0.4 


1053.3 


+35.3 


0.7 










0658.6 


+33.4 


0.7 
















0662.5 


+34.3 


0.5 
















0927.9 


+33.9 


0.3 
















0955.7 


+36.2 
+34.7 


0.3 
±0.4 




+35.6 


±0.4 








HD 75935 


0207.8 


-19.8 


0.4 


1052.3 


-19.3 


0.8 










0308.6 


-19.8 


0.5 


1053.4 


-20.4 


1.0 










0624.8 


-19.1 


0.4 


1055.3 


-18.9 


0.5 










0641.8 


-16.9 


0.8 
















0700.6 


-18.8 


1.2 
















1015.6 


-17.9 


0.9 
















1020.6 


-18.2 
-18.6 


0.6 
±0.4 




-19.5 


±0.4 








HD 86801 


0269.8 


-14.3 


0.5 


1052.4 


-13.0 


0.7 


0943.0 


-12.7 


0.6 




0273.8 


-15.6 


0.7 


1052.4 


-14.9 


0.7 


1026.8 


-17.1 


0.4 




0318.6 


-14.5 


0.6 


1053.4 


-15.7 


0.9 


1035.8 


-13.6 


0.5 




0665.7 


-12.6 


0.6 








1075.7 


-14.8 


0.4 




0971.9 


-16.8 


0.6 
















1015.7 


-12.4 


0.9 
















1022.7 


-15.4 


0.8 















14.5 ±0.7 



-14.5 ±0.8 



-14.5 ±1.0 



120 



John F. Heard and Ch. Fehrenbach 





TABLE U -continued 




STAR 


DAVID DUNLAP HAUTE PROVENCE 


DOMINION ASTROPHYSICAL 




J.D. Vel. J.D. Vel. 
244. . . km/sec ^ ^ 244. . . km/sec ^ ^ 


J.D. Vel. 
244. . . km /sec ^ 



HD 90861 


0208.9 


+36.2 


0.4 


1051.4 


+37.7 


1.3 










0579.9 


+36.4 


0.3 


1051.4 


+36.4 


0.8 










0583.9 


+36.7 


0.3 


1051.4 


+36.5 


0.8 










0592.9 


+36.3 


0.3 


1055.4 


+34.2 


1.0 










0657.7 


+36.9 


0.3 
















0694.6 


+38.8 


0.6 
















0928.0 


+33.5 
+36.4 


0.5 
±0.6 




+36.2 


±0.7 








HD 102494 


0208.0 


-22.3 


0.4 


1051.4 


-21.6 


0.8 


9902.9* 


-24.8 


0.6 




0209.0 


-22.8 


0.3 


1051.4 


-21.7 


1.2 


9993.9* 


-24.0 


0.4 




0257.7 


-24.9 


0.5 


1055.4 


-21.6 


0.5 


0245.0 


-21.7 


0.5 




0951.9 


-24.3 


0.6 


1101.4 


-22.4 


0.7 


1044.8 


-22.9 


0.5 




0967.9 


-23.4 


0.4 


1110.4 


-23.4 


1.0 


1063.9 


-22.1 


0.6 




1024.8 


-21.8 


1.2 








1068.7 


-22.5 


0.7 




1027.8 


-24.1 


0.9 















-23.4 ±0.4 



-22.1 0.3 



-23.0 ±0.4 



112299 


0260.0 


+6.8 


0.6 


1100.4 


+3.0 


0.6 


0724.8 


+3.3 


0.4 




0266.7 


+ 1.9 


0.5 


1101.4 


+3.1 


0.6 


1029.9 


+3.1 


0.5 




0268.8 


+5.0 


0.6 


1134.4 


+2.3 


0.6 










0308.7 


+3.8 


0.4 
















0681.7 


+1.4 


0.9 
















0713.6 


+2.3 


1.0 
















0724.6 


+ 1.3 


1.0 
















0726.6 


+7.0 


0.9 















±3.7 ±0.8 



+2.8 ±0.3 



+3.2 ±0.2 



HD 122693 


0268.9 


-4.8 


0.3 


1100.5 


-7.3 


0.7 


9999.8* 


-6.6 


0.4 




0584.0 


-6.5 


0.5 


1101.5 


-5.2 


0.5 


1068.8 


-5.7 


0.5 




0606.9 


-7.2 


1.2 


1102.4 


-7.0 


0.5 










0657.8 


-6.4 


0.3 


1111.4 


-7.3 


0.7 










0710.8 


-6.7 


0.7 
















0725.8 


-5.5 


0.4 
















1035.8 


-5.5 


0.6 


















-6.1 


±0.4 




-6.7 


±0.5 




-6.2 


±0.5 


HD 132737 


0270.8 


-24.9 


0.4 


1101.5 


-24.0 


0.7 


0734.7 


-22.5 


0.7 




0304.0 


-24.8 


0.5 


1111.4 


-23.6 


0.8 


1068.8 


-27.4 


0.6 




0624.9 


-24.4 


0.3 


1136.4 


-24.0 


1.0 










0657.9 


-24.9 


0.4 


1143.4 


-23.5 


0.8 










0726.7 


-23.8 


2.2 
















0727.6 


-23.2 


0.5 
















0743.7 


-22.7 


0.4 















-24.1 ±0.3 



-23.8 ±0.1 



-25.0 ±1.9 



*J.D. 243 . . 



21 New 9 th Magnitude I A U Standard Radial Velocity Stars 



121 



TABLE \\— continued 



STAR 


DAVID DUNLAP 


HAUTE PROVENCE DOMINION ASTROPHYSICAL 




J.D. 


Vel. 




J.D. 


Vel. 




J.D. Vel. 






244. . . 1 


km /sec 


^ 1 


244. . . 1 


km/sec 


^ 1 


244. . . km/sec 


£ 1 


HD 140913 


0308.9 


-21.2 


0.6 


1110.5 


-18.0 


0.4 


9999.8* -22.3 


0.7 




0681.8 


-19.1 


0.7 


1111.4 


-18.1 


0.4 








0724.8 


-22.6 


0.8 


1134.4 


-21.5 


0.7 








0734.7 


-20.1 


0.6 


1141.4 


-20.8 


0.7 








0746.6 


-21.1 


0.6 


1142.4 


-21.9 


0.8 








0750.6 


-20.8 


0.4 














1022.9 


-22.8 


0.7 
















-21.1 


±0.5 




-20.1 


±0.8 


-22.3 




HD 149803 


0303.9 


-7.0 


0.6 


1147.4 


-9.2 


0.7 


0734.9 -6.1 


0.9 




0367.8 


-7.0 


0.6 


1148.4 


-8.0 


0.5 








0734.8 


-9.7 


0.6 


1149.4 


-8.9 


0.6 








0735.7 


-8.0 


0.6 














0745.7 


-8.3 


0.7 














0760.6 


-4.6 


0.4 














1015.9 


-6.9 


0.6 
















-7.4 


±0.6 




-8.7 


0.4 


-6.1 




HD 160952 


0368.7 


+20.9 


0.5 


1110.5 


+22.5 


0.9 


9999.9* +22.4 


0.4 


jyhjgniy 


0444.7 


+29.1 


0.6 


1111.5 


+23.2 


0.9 






+29037' 


0453.6 


+29.2 


0.7 


1134.5 


+24.8 


0.7 






9.04 


0455.6 


+28.7 


0.3 


1136.4 


+24.2 


0.9 






G8 III 


0736.7 
0759.6 


+24.6 
+23.5 


0.4 
0.5 













Var. 



HD 171232 0116.6 -35.2 0.3 0855.4 -36.9 0.5 



0410.7 


-36.5 


0.6 


0865.3 


-37.8 


0.4 


0413.8 


-38.2 


0.4 


0866.4 


-36.7 


0.6 


0727.7 


-33.6 


0.3 


1111.5 


-36.0 


0.9 


0735.8 


-38.9 


0.6 


1136.4 


-32.4 


0.9 


0746.8 


-34.2 


0.6 








0751.7 


-35.1 


0.5 








0758.7 


-35.6 


0.4 










-35.9 


±0.7 




-36.0 


±0.9 


BD+28O3402 0504.5 


-37.7 


0.7 








0525.5 


-37.1 


0.6 








0759.7 


-36.6 


0.5 








0760.7 


-33.8 


0.9 








0793.7 


-37.1 


0.7 








0800.6 


-36.2 


0.4 








0804.7 


-37.5 


0.6 









-36.6 ±0.5 



*J.D. 243 



122 



John F. Heard and Ch. Fehrenbach 



TABLE W— continued 



STAR 



DAVID DUNLAP HAUTE PROVENCE DOMINION ASTROPHYSICAL 



J.D. 


Vel. 




J.D. Vel. 


J.D 


244. . . 


km /sec 


£l 


244. . . km /sec 


^' 244. 


HD 194071 0418.7 


-9.5 


0.5 


0857.4 -9.1 


0.4 


0425.7 


-9.8 


0.4 


0861.4 -9.6 


0.6 


0751.8 


-9.8 


0.3 


0865.4 -9.9 


0.3 


0758.8 


-9.6 


0.5 


1136.5 -10.6 


0.9 


0773.7 


-8.9 


0.3 


1138.6 -11.0 


0.8 


0774.7 


-10.2 


0.4 






0834.6 


-9.3 


0.5 







Vel. 
km/sec 



El 



-9.6 ±0.2 



-1 0.0 0.3 



HD 204934 0546.5 



-3.3 0.4 0873.3 -11.7 0.4 



21^29^.0 


0547.5 


-6.3 


0.7 


1134.5 


-6.6 


1.1 


+28O09' 


0806.7 


+0.4 


0.3 


1191.3 


-4.7 


0.8 


Ki in 


0861.7 


-11.5 
Var. 


0.9 




Var. 




HD 213947 


0116.7 


+16.7 


0.3 


0852.5 


+18.2 


0.7 




0504.6 


+17.3 


0.6 


0856.4 


+ 15.8 


0.5 




0525.6 


+15.7 


0.6 


0864.4 


+ 16.4 


0.6 




0759.8 


+ 16.1 


0.5 


0893.3 


+ 17.3 


0.6 




0774.8 


+16.8 


0.6 


1134.6 


+18.7 


1.5 




0762.7 


+14.6 


0.6 


1136.6 


+17.4 


1.3 






+16.2 


±0.4 




+ 17.3 


±0.4 


HD 223094 


0116.8 


+19.5 


0.4 


0864.4 


+20.0 


0.6 




0504.7 


+19.7 


0.7 


0864.5 


+ 19.8 


0.9 




0525.7 


+19.6 


0.2 


0866.4 


+21.0 


0.6 




0532.6 


+19.1 


0.4 


0867.4 


+18.9 


0.7 




0576.5 


+16.8 


1.2 


0874.4 


+20.0 


0.6 




0784.8 


+21.9 


0.3 


1134.6 


+ 18.8 


1.1 




0806.8 


+19.9 


0.5 









0479.9 +16.3 0.9 



+ 16.3 



+ 19.5 ±0.6 



+ 19.8 ±0.3 



21 New 9 th Magnitude I A U Standard Radial Velocity Stars 1 23 



TABLE III 

21 NEW lAU STANDARD VELOCITY STARS 



HD or BD 


Q:(1950) 


5(1950) 


Ptg. 


Sp. 


Vel. 


M.E. 


No. of 




h m 


O 1 


Mag. 




km /sec 




Obs. 


4388 


00 43.8 


+30 41 


8.80 


K3 ill 


-28.3 


0.6 


10 


12029 


01 55.8 


+29 08 


8.96 


K2III 


+38.6 


0.5 


12 


14969 


02 22.6 


+29 39 


8.96 


K3 III 


-33.4 


0.3 


10 


23169 


03 40.9 


+25 34 


9.39 


G2 V 


+13.3 


0.2 


13 


32963 


05 04.8 


+26 16 


8.36 


G2 V 


63.1 


0.4 


13 


42397 


06 08.5 


+25 01 


8.68 


GO IV 


+37.4 


0.4 


12 


65934 


07 59.1 


+26 47 


8.87 


G8I1I 


+35.0 


0.3 


10 


75935 


08 50.9 


+27 06 


9.35 


G8 V 


-18.9 


0.3 


10 


86801 


09 58.7 


+28 48 


9.48 


GOV 


-14.5 


0.4 


14 


90861 


10 27.1 


+28 50 


8.36 


K2 III 


+36.3 


0.4 


11 


102494 


11 45.3 


+27 37 


8.26 


G8IV 


-22.9 


0.3 


18 


112299 


12 53.0 


+26 01 


9.19 


F8 V 


+ 3.4 


0.5 


13 


122693 


14 00.5 


+24 48 


8.74 


F8 V 


- 6.3 


0.2 


13 


132737 


14 57.7 


+27 21 


9.03 


KO III 


-24.1 


0.3 


13 


140913 


1543.1 


+28 37 


8.81 


GOV 


-20.8 


0.4 


13 


149803 


16 33.9 


+29 51 


8.90 


F7 V 


- 7.6 


0.4 


11 


171232 


18 30.6 


+25 27 


8.66 


G8III 


-35.9 


0.5 


13 


28° 3402 


19 33.0 


+28 59 


9.55 


F7 V 


-36.6 


0.5 


7 


194071 


20 20.5 


+28 05 


9.06 


G8 III 


9.8 


0.1 


12 


213947 


22 32.3 


+26 20 


8.93 


K4 III 


+ 16.7 


0.3 


13 


223094 


23 43.9 


+28 26 


8.97 


K5 III 


+ 19.6- 


0.3 


13 



David Dunlap Observatory, 
Richmond Hill, Ontario, 
October, 1972. 



PUBLICATIONS OF 

THE DAVID DUNLAP OBSERVATORY 

UNIVERSITY OF TORONTO 



Volume 3 Number 6 



A THIRD CATALOGUE OF 

VARIABLE STARS IN GLOBULAR CLUSTERS 

COMPRISING 2119 ENTRIES 



BY 



HELEN SAWYER HOGG 



973 



PUBLICATIONS OF 

THE DAVID DUNLAP OBSERVATORY 

UNIVERSITY OF TORONTO 



Volume 3 Number 6 



A THIRD CATALOGUE OF 

VARIABLE STARS IN GLOBULAR CLUSTERS 

COMPRISING 2119 ENTRIES 



BY 



HELEN SAWYER HOGG 



1973 



Printed by University of Toronto Press 



INTRODUCTION 

This is the third in the seriesof catalogues of variable stars in globular clusters published 
by the David Dunlap Observatory. The first appeared in 1939 (David Dunlap Publications, 
vol. 1, no. 4) and the second in 1955 (vol. 2, no. 2). In addition, a catalogue of variables 
in globular clusters south of 29° declination was published in 1966 at Cordoba by 
C. R. Fourcade and J. R. Laborde, along with a splendid atlas of photographic prints of 
clusters prepared by J. Albarracin. 

A preliminary edition of this Third Catalogue, in manuscript form, comprising 2057 
entries, was circulated at the lAU Colloquium no. 21, "Variable Stars in Globular Clus- 
ters and in Related Systems." in August 1972. Investigators were invited to send correc- 
tions and additions to the author of the manuscript by October 2, 1972. The cut-off 
date for material included in this publication is November 1, 1972. Considerable new 
material was received, much of it from the Colloquium itself. This led to extensive re- 
visions in the manuscript and some delay in its publication. Some of the conclusions 
drawn from the material of the Third Catalogue are in press in the Colloquium volume 
edited by J. D. Fernie. 

SUMMARY 01 DATA ON VARIABLES IN GLOBULAR CLUSTERS 

At present a recorded search for variables in 108 of the approximately 130 globular 
clusters belonging to our galaxy has been made. This search has yielded 2119 variables. 
Certainly variables do not abound in most globular clusters. Of the 108 clusters that 
have been examined, only 10 contain more than 50 variables each, and 81 contain 
fewer than 20 variables each. At the time of compilation of the Second Catalogue, 
from the distribution it appeared that the most frequent number of variables found in 
a globular cluster was one. Now, from the data in the Third Catalogue, the most fre- 
quent number is zero. There are effectively 13 clusters with no variables, if one includes 
NGC 6397, whose three variables are considered field stars. One variable alone is found 
in each of 10 clusters. 

Figure 1 siiows the frequency distribution of the number of variables per cluster. 
More than 60 per cent of the clusters examined, 65 in all, have 10 variables or fewer; 
exactly 25 per cent, 26 clusters, have more than 20 variables; and 5 clusters have ap- 
proximately 100 or more. The richest cluster still remains NGC 5272, Messier 3, with 
212 variables. The second richest is Omega Centauri, NGC 5139, with 179. Next in 
order of richness is IC 4499, a newcomer in this catalogue, less than 1 0° from the 
southern celestial pole, with 129 discovered by Fourcade and Laborde, and 41 sus- 
pected. Messier 1 5, NGC 7078, with 1 I 1 and Messier 5, NGC 5904, with 97 complete 
this list of exceptionally rich clusters. 

One of the problems faced in compiling this catalogue was to decide whether to in- 
clude or exclude field variables. In general my policy has been to number those varia- 
bles which lie within the obvious confines of a cluster, even though some of them arc 
manifestly field stars. To omit them would ultimately lead to confusion. On the other 
hand, work of recent years in the surroundings of globular clusters has shown that 



Variable Stars in Globular Clusters 



13 
12 
11 

cr 
t^ 9 

3 8 

u 

o ' 

CO 

1 ^ 

^ 4 

3 

2 - 
1 - 



FREQUENCY OF VARIABLE STARS 
IN GLOBULAR CLUSTERS 
1972 



NGC 5272 1212)- 

NGC 5139 (179)- 

IC 4499(1291- 

NGC 7078 (111)- 



"^ \ r 

50 60 70 

OF VARIABLES 



10 



20 



30 40 

NUMBER 



80 



90 



100 



Figure 1 Distribution of the known, published variables per cluster. 

some of the RR Lyrae stars well beyt)nd their confines are likely members, or were so 
in the past. These stars are not included among the numbered variables of a cluster, ex- 
cept in a few cases. 

NUMBERS OF TYPES OF VARIABLES AND KNOWN PIRIODS 

Of the known variables, periods have now been determined for 1313 in 55 clusters, 
compared with 843 in 38 clusters in 1955. In many clusters some periods have been 
revised or redetermined. In some cases there are only minor changes in the fifth or 
higher decimal places, but in others the change is major, even in the first decimal, 
giving an alternate period. In addition, many determinations of period changes have 
now been made. An effective summary of such changes in a concise catalogue is not 
possible, and the reader is referred to the original papers t\)r pertinent data. 

Table I gives a summary of the numbers and types of variables and numbers oi 
periods known in the 108 globular clusters for which there is a record of search. For 
further particulars about these stars, such as cluster membership, the reader is referred 
to the catalogue itself. 

The first column of the table gives the customary designation of the cluster, usually 
the NGC number. The second gives the total number of variables, and the third the 
total number of known periods. Periods for RR Lyrae stars are counted as known even 
when the published value is questionable or there is an alternate period, providing at 
least two decimals are given; and for semircgular variables if a numerical value of the 
cycle has been published. The fourth column gives the number of RR Lyrae periods 



Introduction 

TABLE I 

Summary of Variable Stars in Globular Clusters 





Total 


Total 


RRLyr 


1-30 


31-99 


100-220 


>220 


Irr 




NGC 


variables 


periods 


periods 


days 


days 


days 


days 


SR 


Others 


104 


28 


10 


2 




3 


5 




4 




288 


1 


1 








1 








362 


15 


10 


7 


2 


1 










1261 


15 



















Pal 1 





















Pal 2 





















1851 


10 



















1904 


7 


3 


3 










1 




2298 


2 



















2419 


36 















5 




2808 


9 



















Pal 3 


1 



















3201 


88 


84 


83 












EA, mem.' 


Pal 4 


2 


2 








2 








4147 


16 


15 


15 














4372 


2 



















4590 


42 


38 


37 








IF 






4833 


16 


9 


6 




1 




21 


1 




5024 


47 


36 


33 


1 


1 


1 








5053 


11 


10 


10 














5139 


179 


159 


142 


7 


5 


2 


IF 


3 


3E, 1 RRs 


5272 


212 


186 


182 


1 


2 


1 






1 EW 


5286 


8 



















5466 


23 


21 


21 














5634 


7 


1 


1 














5694 





















14499 


129 



















5824 


27 


9 


9 








1 






Pal 5 


5 


5 


5 














5897 


7 


7 


6 




1 










5904 


97 


92 


90 


2 








1 


1 UG 


5927 


11 


1 










1 






5946 


3 



















5986 


5 



















6093 


8 


3 




1 




IF 


IF 




1 N 


6101 





















6121 


43 


42 


40 




2 










6139 





















6144 


1 



















6171 


25 


23 


22 








IF 






6205 


11 


7 


3 


3M 


1 M 






2M 


1 F 


6218 


1 


1 




1 












6229 


22 


15 


14 


1 












6235 


2 




















Variable Stars in Globular Clusters 





Total 


Total 


RRLyr 


1-30 


31-99 


100-220 


>220 


Irr 


NGC 


variables 


periods 


periods 


days 


days 


days 


days 


SR 


Table I (continued) 














6254 


4 


2 




2 








1 


Palis 



















6266 


89 


74 


74 












6273 


4 

















6284 


6 

















6287 


3 

















6293 


5 

















6304 


21 

















6333 


13 


11 


11 












6341 


15 


13 


12 












6352 


4 

















6356 


10 


1 








1 






6362 


33 


15 


15 












6366 


2 

















HP 1 


15 

















6380 


1 

















6388 


9 
















Ton 2 


2 

















6397 


3 


3 


IF 




IF 




IF 




6401 


3 

















6402 


77 


40 


34 


5 






IF 




Pal 6 



















6426 


13 


11 


11 












6441 


10 

















6453 



















6496 



















6522 


10 


9 


8 


IF 








IF 


6528 



















6535 


1 

















6539 


lu 

















6541 


1 

















6553 


18 


4 


3 








1 




6558 


9 

















11276 


5 


1 


1 










4? 


6569 


5 

















6584 


1 

















6624 


4 

















6626 


18 


10 


7 


2 


1 








6637 


8 


2 








2M 






6638 


3 

















6642 


2 

















6652 



















6656 


32 


27 


18 


IM 


2 


2F? 


4F? 


IW 


6681 


2 

















6712 


21 


16 


10 






6 






6715 


80 


37 


34 


1 


1 


1 







Others 



1 EWF 



IN 



Slow, prob. mem 
2 slow, 1 N 



1 RR F, 2 red giant 



1 UG, 2 E F? 

2 E, 2 SR, 3 F 











Introduction 






5 




Total 


Total 


RR Lyr 


1-30 


31-99 100-220 


>220 


In- 




NGC 


variables 


periods 


periods 


days 


days days 


days 


SR 


Others 


Table I (continued) 














6723 


25 


19 


19 












6752 


2 

















6760 


4 

















6779 


12 


4 


IF 


1 


1 




6 


1 RRsF? 


Pal 10 


1 

















6809 


6 


5 


5 












Pain 



















6838 


4 


2 






1 




1 


1 EA, mem 


6864 


11 

















6934 


51 


30 


30 










1 slow 


6981 


40 


28 


28 












7006 


71 


58 


57 




1 








7078 


111 


68 


65 


3 










7089 


21 


21 


17 


3 


1 








7099 


12 


4 


3 










lUG 


Pall 2 


3 

















Pal 13 


4 


4 


4 












7492 


4 


4 


3 


1 











determined. The next three columns cover the period interval between the RR Lyrae 
and the Mira stars with periods greater than 220 days. The totals in this period interval 
are broken down arbitrarily into three groups. The shorter group is made up mainly of 
W Vir stars, and the longer of short-period Mira stars, with semiregular or RV Tauri 
types in between. Only those variables technically in the pulsating variable group are 
included in the above-mentioned columns. Others, mainly eclipsing, are noted in the 
last column of the table. Mira stars with periods over 220 days are in the eighth col- 
umn. These are mainly field stars. The ninth column contains those variables with no 
period given, mainly red ones, with irregular or semiregular fluctuations. 

About 8 per cent of the stars in the catalogue, 169 in all, are definitely designated as 
other than RR Lyrae. There are 39 in the 1-30 day group, 26 in the 31-99, 26 in the 
100-219, and 15 with a period of over 220 days. A conspicuous difference between the 
Third and Second Catalogues is the increase in the number of red irregular variables, 
many with small ranges. 



DISTRIBUTIONS OF RR LYRAE PERIODS 

There are 1202 definite RR Lyrae periods known in 46 clusters. The importance of the 
difference in most frequent length of period in individual clusters has been widely dis- 
cussed since Oosterhoff first called attention to it. Figure 2 shows the distribution of 
all RR Lyrae periods in globular clusters for period intervals of 0.01 day. The double 
maximum of this distribution, conspicuous in the Second Catalogue, is further en- 



Variable Stars in Globular Clusters 




Figure 2 Numbers of RR Lyrae periods at intervals of 0.01 days. 

hanced by the new material. Certainly in globular clusters variables of the RRab type 
have a strong preference for periods around 0.55 day, and of the RRc type, around 
0.35 day. 



DESCRIPTION OF THE CATALOGUE 

The catalogue contains every globular cluster considered as belonging to our galaxy for 
which there is now a published record of search for variables. These clusters number 
108, and 1 1 others are mentioned in brief references. 

For the material of the catalogue an attempt has been made to select the most recent 
or the best determined data. This means that in some clusters for even a single variable 
the data in different columns may be drawn from different sources. When the Second 
Catalogue was prepared in 1955, every effort was made to obtain from the authors, or 
their respective institutions, information sufficient to identify variables listed many 
years earlier as unpublished. Despite this attempt, much of the unpublished material 
had to be left in relatively useless form. Now, 17 years later, it seems unlikely that any 
more of this material can ever be salvaged, and in most cases it is not mentioned in the 
Third Catalogue. 

The system of references has been put on a different basis from that used in the First 
and Second Catalogues. As the literature proliferates with the years, it becomes no 
longer feasible to reprint all the references for a cluster in each catalogue. Accordingly 



Introduction 7 

only references since the publication of the Second Catalogue are included for the 
most part, along with a few overlooked earlier. However, for some clusters on which 
there has been no key work since then, an occasional early reference has been repeated 
to aid the reader. 

The format of the reference system has also been altered from that used in the earlier 
catalogues. References are now printed under each cluster. The abbreviations of publi- 
cations have been chosen to conform to the system of H. Schneller in Geschichte und 
Literaturdes Lichtwechsels der Veranderlichen Sterne (Berlin), which seems to convey 
the necessary information in as concise a manner as possible. An index of the abbrevia- 
tions used is given at the end of the catalogue. Photo or chart is shown by (p) or (c). 

The principal papers on variables in any cluster are listed by author and abbreviated 
reference. However, there are some papers (23 in all) with remarks about many clusters. 
These more frequently mentioned papers are abbreviated to initials and the year of pub- 
lication in this century, the key to these abbreviations being also given at the end, with 
the title of the paper. For clusters for which the Atlas and Catalogue of Fourcade, La- 
borde, and Albarracin contains new material, this reference is listed with the main ref- 
erences; otherwise it appears among the highly abbreviated ones. 

Anyone actually investigating a cluster is strongly urged to consult the full list of ref- 
erences given in the Second Catalogue. 

The clusters are Hsted in order of NGC number, which does not always correspond to 
the order in right ascension. Those lacking an NGC number are placed in order of right 
ascension, which, along with declination, is given for the equinox of 1950. If the cluster 
has a Messier number, that is given. 

The variables are numbered according to the previous catalogues, and new numbers 
are usually assigned in order of discovery. The policy is to try to restrict the new num- 
bers to those variables within the apparent physical area of the cluster, but it is not 
feasible to follow this rule rigidly. 

Thejc and>' coordinates are given in seconds of arc and correspond in direction to 
right ascension and declination. For a given cluster, they are usually those pubhshed by 
the first investigator, or reduced to his selected centre. In some cases, these coordinates 
unfortunately are not yet available. 

The magnitudes are usually the latest that have been obtained, which are hopefully 
the best determined for maximum and minimum. Most of the magnitudes are photo- 
graphic, but there is a gradual shift to the use of B magnitudes. 

The epoch of maximum is usually, but not always, chosen as the one accompanying 
the period selected. Individual papers should be consulted to determine whether the 
time is heliocentric or geocentric. 

The period is generally that most recently published. Stars with periods less than a 
day are assumed to be of RR Lyrae type unless otherwise indicated in the remarks. For 
stars with periods between one and thirty days the type is assumed to be Cepheid. 

The "remarks" column contains a miscellany of information. An increase or decrease 
in period is indicated by + or - respectively, a constant period by "est" or 0. "Alt" 
means an alternate period has been published, "var" signifies a variable period, and "B2" 



8 Variable Stars in Globular Clusters 

the Blashko effect. An available spectral type is indicated by "Sp" sometimes followed 
by the type without subdivision, and an available radial velocity by "V." Stars which 
have been shown to be definitely or very probably field stars are indicated by "f " and 
proven cluster stars by "mem." The abbreviation used for the type of variable is that in 
the Third Edition of the General Catalogue of Variable Stars by B. V. Kukarkin et al. 
(1969). For variables found since publication of the Second Catalogue, the discoverer 
is usually indicated. 

ACKNOWLEDGMENTS 

It is a pleasure to acknowledge the help I have received in the construction of this cata- 
logue. This has come from many astronomers who have sent unpublished or explanatory 
data, as indicated in the references under individual clusters. I am particularly grateful 
to Professor Dr. B. V. Kukarkin of Moscow University, who, in the midst of his great 
task of recording all galactic system variables, has taken time to keep me briefed on 
Soviet work in globular clusters and to send me corrections to some of my previous 
papers. Also Dr. H. Wilkens of Argentina has been a constructive reader of my past 
works, and Dr. Steven van Agt of Nijmegen has straightened out the material on NGC 
6362. 

My thanks go also to the two directors of this observatory under which the Third 
Catalogue has been compiled. Dr. John F. Heard and Dr. Donald A. MacRae; to the 
National Research Council of Canada for their generous support of my cluster pro- 
gram; to my colleagues Dr. Amelia Wehlau of the University of Western Ontario and 
Dr. Christine Coutts; to the two librarians who assiduously tracked down elusive refer- 
ences, Mrs. Jean Lehmann and Mrs. Sheila Smolkin; to Mrs. Jennie Fabian, who pre- 
pared the preliminary version for distribution at lAU Colloquium no. 21 in August 
1972; and last but not least to my daughter, Mrs. Sally MacDonald, who searched ref- 
erences and tabulated data. 

June 30, 1973 
Richmond Hill, Ontario 



THIRD CATALOGUE OF VARIABLE STARS 
IN GLOBULAR CLUSTERS 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC 104 (47 Tucanae) a0d^2l"^.9, 6-72°21' 



1 
2 
3 
4 
5 
6 
7 
8 
9 

10 
11 
12 
13 
14 
15 
16 
17 
18 
19 
20 
21 
22 
23 
24 
25 
26 
27 
28 



36.8 
64.7 
328.4 
18.8 
271.9 
97.3 
349.2 
16.0 
108 
72 
306 
+ 1254 
- 301.95 
+ 8.25 



-112.6 

-193.9 

+ 52.8 

-160.4 

-284.6 

-103.8 

-113.0 

+ 57.0 

- 78 

+702 

+ 138 

-348 

-139.92 

+ 66.83 



11.60 15.63 

11.70 14.48 

11.70 15.85 

12.50 14.0 

13.0 13.7 

13.0 13.6 

13.0 13.7 
12.4 14.0 
13.6 14.7 

13.1 13.6 

13.2 14.0 

13.89 14.45 36046.614 



12.0 


12.3 


11.0 


11.6 


11.7 


12.5 


12.0 


13.0 


11.7 


12.2 


11.7 


12.2 


11.6 


11.9 


11.6 


11.9 


11.8: 


12.1: 


11.9 


12.2 


11.8 


12.2 



35487 
35645 
35468 
35490 
36158 
36159 
36162 
35524 
36163.240 



212 
203 
192 
165 

45 

47 

58 
155 

0.73652 
irr 
irr 

0.37143 



SpM, V 
SpM,V 
SpM, V 

SpM,V 

SpM,V 
SpM, V 
mem, Sp, V 



f, Sp, V 

Wilkens 

F&L 

W300 

R18 

W81 

L168 

RIO 

Al 

A2 

A4 

A6 

A8 

A9 

A13 

A18 

LR5 



V15 found by Eggen, 1961; V17 Eggen, 1972; V16 Brooke, 1969. Unpublished V magnitudes given 
for vars. 18-28, discovered by Lloyd Evans and Menzies, marked on print (1973); their identifying 
numbers are given in the remarks column. W = Wildey (1961), R = Feast and Thackeray (1960). A 
field variable, HV 809, is shown by Jones (1973) to be a non-member. 

Feast, Thackeray and Wessehnk, MN 120.64(1960); Feast and Thackeray, MN 120.463 (1960); 
Eggen, Royal Obs Bull 29.E86 (1961); Kurochkin, VS 13.248 (1961); Wildey, ApJ 133.430 (p) 
(1961); Rosino and Sawyer Hogg, lAU Trans 118.301 (1962); Arp, Brueckel and Lourens, ApJ 
137.228 (1963); Feast, ApJ 137.342 (1963); Tifft, MN 126.210 (1963); Fourcade, Laborde and 
Albarracin, Atlas y Catalogo, Cordoba (1966); Brooke, Doctoral Thesis, Australian Nat'l Univ 
(1969); Eggen, ApJ 172.639 (1972); Lloyd Evans, Letter (1972); Jones, lAU Coll 21 (1973); 
Lloyd Evans and Menzies, lAU Coll 21 (p) (1973) 

S55a, S57, S59, S61, A62, R62a, S62, P64, S64, R65, S69, F72 



10 



Variable Stars in Globular Clusters 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC 288 a 00h50'".2, 5 -26° 5 2' 
1 -55 +79 13.5 



14.1 



25576 



103 



Shapley, Star Clusters, p. 45 (1930); Oosterhoff, BAN 9.397 (1943) 
S55a, S59, R62c, S62, S69 



NGC 362 a Ol^Ol^^.e, 5 -71°07' 



1 


-246.2 


- 67.6 


14.9 


16.1 


23751.558 


0.5850512 


2 


+ 41.4 


-204.4 


13.0 


14.5 


24391.8 


90var 


3 


+ 93.6 


-143.2 


14.6 


16.1 


23604.806 


0.4744151 


4 


- 50.2 


- 27.3 


14.0 


15.8 






5 


- 79.2 


- 31.9 


15.1 


16.4 


24025.729 


0.4900846 


6 


+ 82.4 


+ 15.5 


14.9 


16.3 


24461.642 


0.5146080 


7 


+ 131.1 


- 21.2 


14.8 


16.0 


24468.687 


0.5285492 


8 


+ 33.4 


-308.5 


15.0 


16.5 


24433.677 


3.901447 


9 


-400.4 


+ 224.4 


14.7 


16.0 


24404.670 


0.5476126 


10 


+ 282.8 


-381.8 


14.9 


16.4 


23315.643 


4.20519 


11 


-136.1 


- 26.0 


15.1 


16.0 






12 


- 30.4 


-115.4 


15.2 


16.1 


24391.839 


0.6525451 


13 


+ 14.5 


+ 38.8 


14.6 


16.3 






14 


- 23.8 


- 66.8 


14.8 


16.2 






15 


+ 151.3 


-210.7 











F&L 

Bailey, HA 38.237 (p) (1902); Sawyer, HC 366 (1931), HC 374 (p) (1932); Kurochkin, VS 13.248 
(1961); Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966); Eggen, ApJ 172.639 
(1972) 
S55a, S59, S62, S64, L65, R65, S69 

NGC126I al3hloni.9, 5-55°25' 

L&F 

L&F 

L&F 

L&F 

L&F 

L&F 

L&F 

L&F 

L&F 

L&F 

L&F 

Bartolini 

Bartolini 

Bartolini 

Bartolini 

Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966); Laborde and Fourcade, 
Cordoba Repr 127 (1966); Bartolini, Grilli and Robertson, IBVS 594 (1971); Bartolini, Grilli and 
Morisi, IBVS 649 (1972); Bartolini, Letter (1972) 
S55b, R62b, S67, S69 



1 


- 29.8 


- 28.4 






2 


- 39.8 


+ 34.9 


16.05 


17.25 


3 


+ 49.6 


- 54.6 


15.88 


16.67 


4 


+ 31.8 


- 36.1 






5 


- 34.5 


- 5.0 


16.1 


17.0 


6 


+ 78.1 


- 12.3 


16.32 


17.32 


7 


-149.3 


+ 140.2 


16.85 


17.3 


8 


-133.7 


-139.0 


16.13 


17.48 


9 


+ 37.9 


- 38.8 


16.85 


17.15 


10 


+ 52.3 


+ 70.6 


16.17 


17.43 


11 


- 89.0 


+ 89.5 


16.85 


17.29 


12 


+ 87.1 


- 10.5 


16.35 


17.42 


13 


- 77.1 


- 96.0 


16.79 


17.35 


14 


- 53.5 


- 70.7 


16.22 


17.23 


15 


-114.5 


+ 129.1 


15.21 


15.86 



I 



Catalogue 



11 



No. 



Max. Min. 



Epoch 



Period 



Remarks 



Palomar 1 a 03^25^.7, 5 +79° 28' 

No variables found. 

Kinman and Rosino, ASP 74.499 (1962) 

R61, S61 



Palomar 2 a 04^43^.1, 5 +31°23' 

No variables found. 

Rosino and Pinto, lAU Coll 21 (1973) 

R61 



NGC1851 a05hl2m.4, 5-40°05' 



1 


+258.50 


- 12.38 


14.0 


15.5 


2 


- 41.25 


+ 30.25 


14.0 


15.5 


3 


- 38.50 


+ 92.13 






4 


+ 24.75 


+ 35.75 






5 


+ 41.25 


+ 41.25 






6 


- 74.25 


- 8.25 






7 


+ 4.13 


- 8.35 






8 


+ 28.88 


+ 24.75 


var? 




9 


- 57.75 


+ 49.50 







10 



+ 46.75 



196.63 



Small change in coordinates of vars. 1 and 2 discovered by Bailey. Variable formerly noted as un- 
published is considered to be included in above list of new vars. 3-10 discovered by Laborde and 
Fourcade. 

Bailey, HB 802 (1924); Shapley, Star Clusters, p. 45 (1930); Laborde and Fourcade, Cordoba Repr 
138 (p) (1966) 

S55a, S59, R62c, S62, F&L63, FLA 66, S69 



NGC 1904 (Messier 


79) a05h22m.2. 


5 -24° 34' 








1 +29.6 


-199.6 


var? 








med 16.0 


2 +78.3 


- 68.3 


14.2 


14.80 




SR 




3 +34.8 


- 64.4 


15.9 


16.7 


34032.40 


0.73602 




4 +93.4 


- 50.1 


15.6 


16.7 


32877.50 


0.63492 




5 -11.6 


+ 20.2 












6 -70.8 


+ 115.6 


16.0 


16.6 


32940.25 


0.33522 




7 +22.5 


- 15.2 










Tsoo Yu-hua 


8 + 7.1 


11.7 










Tsoo Yu-hua 



Pickering, HC 18 (1897); Bailey, HA 38.238 (p) (1902); Rosino, Bologna Pubbl 5, 20 (p) (1952); 
Tsoo Yu-hua, Letter (p) (1965) 
S55a, S59, S62, L65, R65, S67, S69 



12 Variable Stars in Globular Clusters 



No. x" y" Max. Min. Epoch Period Remarks 

NGC2298 a06h47m.2, 6-35°57' 

1 +119.35 -37.40 F&L 

2 - 30.53 -22.28 F&L 

Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966) 
S55a, S59, R62c, S62, F&L63, S69 

NGC2419 a07h34ni.8, 6+39°00' 



1 


+ 40 


- 52 


17.59 


18.32 


2 


- 4 


- 19 






3 


+ 52 


- 24 


18.66 


19.96 


4 


+ 80 


- 15 


18.84 


19.65 


5 


+ 33 


+ 47 


18.75 


19.72 


6 


+ 56 


-127 


18.86 


19.64 


7 


+ 91 


+ 87 


18.69 


19.77 


8 


- 17 


+ 41 


17.50 


18.10 


9 


- 32 


+ 88 


18.59 


19.76 


10 


+ 20 


- 51 


17.31 


17.93 


11 


+ 95 


- 8 


18.55 


19.81 


12 


+ 133 


+ 111 


18.69 


19.71 


13 


+ 101 


- 10 


18.55 


19.75 


14 


-115 


- 13 


18.81 


19.62 


15 


+ 62 


+ 40 


18.62 


19.76 


16 


+ 47 


+ 72 


18.77 


19.85 


17 


+ 109 


+ 111 


18.65 


19.75 


18 


- 15 


+ 114 


17.84 


18.53 


19 


-107 


- 40 


18.77 


19.86 


20 


- 28 


+ 45 


17.65 


18.16 


21 


- 55 


+ 30 


18.76 


19.74 


22 


+ 109 


- 5 


18.60 


19.84 


23 


+ 27 


+ 79 






24 


-147 


- 10 


18.94 


19.58 


25 


- 59 


+ 38 


18.78 


19.70 


26 


- 70 


- 50 






27 


+ 19 


-103 


19.10 


19.55 


28 


-192 


+ 59 


18.72 


19.78 


29 


- 58 


- 7 


19.01 


19.92 


30 


- 26 


+ 23 






31 


+ 154 


-146 


19.08 


19.53 


32 


- 19 


+ 48 


18.60 


19.71 


33 


+ 47 


- 17 


19.11 


20.13 


34 


+ 21 


+ 157 


19.00 


19.66 


35 


+ 43 


+ 8 


18.88 


20.00 


36 


+ 23 


+ 44 


19.10 


19.83 



Kinman has two RR Lyrae periods, 0.37 and 0.63 days. 

Baade, ApJ 82.396 (p) (1935); Rosino and Sawyer Hogg, lAU Trans 11B.301 (1962) 

S55a, S59, S62, R65,S69 



Catalogue 



13 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC2808 a09hl0m.9, 5-64°39' 

F&L 

F&L 

F&L 

F&L 

F&L 

F&L 

F&L 

Alcaino 27 

Alcaino 35 

Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966); Alcaino, Astr and Ap 15.360 
(P)(1971) 

S55a, S59, R62c, S62, S69 



1 


+ 107.25 


- 35.20 






2 


- 48.13 


+ 34.10 






3 


+ 31.63 


- 61.33 






4 

5 


-191.13 
+ 39.05 


+ 60.50 
- 66.00 






6 


+ 168.58 


-291.50 






7 


+ 63.25 


+ 60.50 






8 






14.87 


15.92 


9 






15.68 


16.96 



PaIomar3 a lOhoS^.O, 5+00° 18' 

VI on print 

Burbidge and Sandage, ApJ 127.5 27 (p) (1958) 
S61, S62, S69 



prob RR 



B&S 



NGC 3201 


aioh 


15^.5, 6 


-46°09' 










1 


+ 


59 


- 118 


14.56 


15.66 


39505.858 


0.6048761 


+ 


2 


+ 


29 


- 117 


14.61 


15.60 


28272.352 


0.5326722 




3 


+ 


182 


- 43 


14.84 


15.52 


39504.76: 


0.5994093 


- 


4 


+ 


155 


+ 3 


14.76 


15.60 


23198.539 


0.6300006 




5 


+ 


42 


- 24 


14.40 


15.54 


39504.853 


0.5015359 


+ 


6 


- 


116 


- 143 


14.42 


15.42 


39506.796 


0.5256131 


- 


7 


- 


91 


- 189 


14.88 


15.40 


39505.823 


0.6303322 


+ 


8 


- 


69 


- 99 


15.06 


15.40 


39504.816 


0.6286280 


+ 


9 


- 


51 


- 91 


14.86 


15.57 


23506.605 


0.5266970 




10 


- 


181 


+ 235 


14.66 


15.59 


22429.597 


0.5351571 




11 


- 


104 


+ 112 


14.82 


15.36 


39506.804 


0.2990471 


+ 


12 


- 


86 


+ 108 


14.50 


15.53 


23547.577 


0.4955583 




13 


- 


160 


+ 92 


14.66 


15.56 


39506.720 


0.5752145 


+ 


14 


- 


156 


+ 133 


14.61 


15.67 


23961.495 


0.5092897 




15 


- 


279 


- 173 


14.34 


15.43 


23164.572 


0.5346644 




16 


- 


197 


- 238 


14.83 


15.21 


39504.819 


0.365 




17 


+ 


11 


- 25 


14.80 


15.52 


39506.874 


0.5655773 


- 


18 


+ 


23 


- 24 


14.73 


15.54 


39504.872 


0.53 




19 


+ 


23 


+ 317 


14.40 


15.50 


39506.821 


0.5250201 


- 


20 


+ 


39 


+ 284 


14.40 


15.52 


39505.816 


0.5291064 


+ 


21 


+ 


94 


+ 135 


14.74 


15.62 


39506.763 


0.5666509 


+ 


22 


- 


100 


- 56 


14.66 


15.57 


39506.825 


0.6059842 


+ 


23 


- 


49 


- 50 


14.75: 


15.12: 


39504.81 


0.61 


Companion 


24 


- 


339 


+ 17 


14.40 


15.52 


39505.869 


0.5889798 


- 


25 


+ 


93 


+ 173 


14.43 


15.47 


39505.818 


0.5147963 


+ 



14 



Variable Stars in Globular Clusters 



No. 




•i" 


y' 




Max. 


Min. 


Epoch 


Period 


Remarks 


NGC 3201 (continued] 














26 


+ 


219 


— 


140 


14.87 


15.70 


39505.878 


0.5689949 


- 


27 


+ 


58 


- 


323 


14.08 


15.32 


39505.790 


0.4842943 


+ 


28 


+ 


66 


- 


48 


14.70 


15.60 


39505.760 


0.5786766 


- 


29 


- 


256 


+ 


113 


15.12 


15.48 


39506.74: 


0.343 




30 


- 


289 


+ 


272 


14.29 


15.49 


39504.814 


0.5158559 


+ 


31 


+ 


182 


+ 


131 


14.65 


15.51 


23505.620 


0.5194894 




32 


+ 


195 


+ 


199 


14.30 


15.54 


39504.900 


0.5611656 


+ 


33 


+ 


48 


- 


40 


not var 










34 


+ 


296 


+ 


285 


14.37 


15.62 


23547.577 


0.4678883 




35 


- 


11 


+ 


121 


14.90 


15.45 


22484.504 


0.6155244 




36 


- 


108 


- 


11 


14.68 


15.2: 


39505.794 


0.242 


Alt 0.323 


37 


- 


68 


- 


74 


15.04 


15.40 


39504.77 


0.273 


Alt 0.382 


38 


- 


61 


- 


60 


14.70 


15.60 


23877.612 


0.5091616 




39 


+ 


41 


+ 


54 


14.83 


15.80 


23181.537 


0.4832092 




40 


- 


96 


+ 


68 


15.10 


15.56: 


39504.90 


0.642 


Alt 0.385 


41 


+ 


291 


+ 


28 




15.55 




0.66 




42 


- 


301 


+ 


197 


14.26 


15.40 


39504.840 


0.5382490 


+ 


43 


- 


377 


+ 


15 


14.80 


15.39 


23166.665 


0.6761289 




44 


+ 


31 


+ 


67 


15.01 


15.66 


23190.635 


0.6107344 




45 


+ 


127 


- 


32 


14.56 


15.60 


39505.859 


0.5374165 


+ 


46 


- 


396 


- 


510 


14.56 


15.35 


23167.570 


0.5431990 




47 


+ 


108 


+ 


245 


14.78 


15.42 


39504.903 


0.342: 


Be, Alt 0.51 


48 


— 


252 


+ 


12 


14.96: 


15.36 


39506.67: 


0.336 


Alt 0.252 


49 


- 


38 


+ 


151 


14.72: 


15.46 


39504.76: 


0.5814870 


+ 


50 


- 


13 


+ 


27 


14.80 


15.72 


39506.88 


0.565 




51 


- 


205 


- 


26 


14.50 


15.30 


39506.813 


0.5 205454 


+ 


52 


+ 


14 


- 


812 


14.90 


15.30 


39505.78: 


0.38: 




53 


- 


873 


- 


758 


14.57 


15.38 


23191.540 


0.5334705 




54 


+ 


671 


- 


804 


14.71 


15.8: 


39506.776 


0.5558721 


+ 


55 


- 


338 


+ 


767 


14.47 


15.43 


39504.915 


0.607 




56 


+ 


246 


+ 


94 


14.95 


15.62 


23164.591 


0.5903376 




57 


+ 


288 


- 


72 


14.74 


15.58 


39506.762 


0.5934373 


+ 


58 


+ 


346 


- 


80 


14.94 


15.45 


23164.538 


0.6220418 




59 


- 


490 


- 


70 


14.28 


15.28 


39506.813 


0.5177106 


+ 


60 


- 


850 


+ 


95 


14.08 


15.38 


39505.798 


0.5035723 


- 


61 


- 


1125 


+ 


175 


14.12 


15.59 


39504.91 


0.54 




62 


- 


1060 


- 


186 


14.29 


15.49 


39505.798 


0.5697558 


- 


63 


— 


1000 


+ 


59 


14.36 


15.39 


23914.582 


0.5680998 




64 


- 


646 


+ 


863 


14.32 


15.54 


39504.815 


0.5224218 


+ 


65 


- 


544 


+ 


797 


14.01 


15.03 


39506.71 


1.660024 


EA,Min, mem? 


66 


— 


398 


+ 


289 


14.90 


15.27 


39506.78 


0.284 




67 


- 


374 


- 


120 


14.75: 


15.31 


39506.70: 


0.329 


Alt 0.494 


68 


- 


283 


+ 


846 








long 




69 


- 


221 


+ 


995 


14.34 


15.50 


23914.575 


0.5122704 




70 


— 


221 


- 


13 


not var 










71 


- 


182 


- 


117 


14.35 


15.39 


39506.765 


0.6011859 


+ 


72 


- 


161 


+ 


596 


15.00 


15.24 




0.36? 





Catalogue 



15 



No. 




x" 


y 


" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC 3201 (continued) 












73 


— 


128 


+ 


86 


14.40 


15.60 


39504.860 


0.5199500 


+ 


74 


- 


94 


+ 


36 


not var 










75 


- 


81 


+ 


147 


not var 










76 


- 


62 


- 


42 


15.16 


15.72 


39506.74 


0.343 


Alt 0.52 


77 


- 


10 


- 


52 


14.64 


15.50 


22429.592 


0.5676648 


- 


78 


- 


8 


- 


143 


14.48 


15.48 


39504.83 


0.514 




79 


+ 


10 


- 


101 


not var 










80 


+ 


60 


+ 


23 


14.82 


15.60 


39505.79 


0.58 




81 


+ 


96 


^ 


153 












82 


+ 


161 


- 


166 


not var 










83 


+ 


177 


+ 


172 


14.44 


15.62 


23190.624 


0.5451918 


- 


84 


+ 


358 


+ 


703 


14.65 


15.43 


22077.566 


0.5136787 




85 


+ 


569 


- 


403 


not var 










86 


+ 


611 


- 


315 


not var 










87 


+ 


1013 


- 


460 


14.65 


15.30 


23164.633 


0.6038866 




88 


+ 


234 


+ ; 


1086 


14.48 


15.61 


39504.86 


0.57 


Wilkens 1 


89 


+ 


1404 


- 


180 


14.90 


15.38 


39505.83 


0.369 


Wilkens 2 


90 


- 


24 


+ 


06 


14.8: 


15.65 


39504.73: 


0.61 


Wilkens 3 


91 


- 


1524 


+ 1170 


14.64 


15.10 


39504.98 


0.345 


Wilkens 4 


92 


- 


150 


- 


30 


14.48 


15.50 


39506.80 


0.523 


Wilkens 5 


93 


+ 1986 


- 


192 








0.48? 


Wilkens 6 


94 


- 


2862 


+ : 


1824 








RR 


Wilkens 7 


95 


+ 


1860 


+2580 








RR 


Wilkens 8 


96 


- 


2790 


- 


468 


14.50 


15.50 


39506.86 


0.59 


Wilkens 9 



Wilkens no. 10 = V39. Kukarkin considers Wilkens' new variables are cluster members, forming a 
large corona, and says identifications of vars. 6, 11, 45, 52, 57, 68 and 81 are erroneous in FLA66. 

Wilkens, MVS 3.75 (1965); Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966); 
Kukarkin, AC 426.4 (1967), AC 428.1 (1967), AC 637.4 (1971), VS 17.610 (1971), Letter (1971) 

S55a, S57, S59, S61, R62a, S62, S64, L65, R65, St66, S67, S69, S70 



Palomar4 a llh26ni.6, 5 +29° 15' 



-12 

-43 



4 


17.7 


20 


35922 


3 


17.6 


19.3 


35938 



130.50 
109.30 



Rosino 
Rosino 



Rosino, Asiago Contr 85 (1957); Burbidge and Sandagc, ApJ 127.527 (1958); Rosino and Pinto, 
IAUCoU21 (1973) 
R57, S59, R61, S61, S62, S69 



NGC 4147 ai: 


>h07m.6, 5 + 


18°49' 










1 -100.1 


- 45.7 


16.36 


17.76 


35546.544 


0.5003860 




2 - 20.2 


- 28.8 


16.46 


17.64 


35538.485 


0.49306 




3 - 28.5 


- 35.3 


16.68 


17.24 


35538.591 


0.280542 




4 + 1 


+ 18 


16.27 


17.29 


34805.859 


0.30097 




5 + 14.9 


+ 2.7 


17.0 


17.4 




0.34125: 


Newburn 


6 + 31.2 


+ 28.4 


16.29 


17.67 


34805.675 


0.61860 


S&W 



16 



Variable Stars in Globular Clusters 



No. 


x" 


y 




Max. 


Min. 


Epoch 


Period 


Remarks 


NGC4147 (cont 


nued) 












7 


+ 4.6 


+ 


7.4 


16.4 


17.6 


34805.924 


0.51294 S&W 


8 


+ 8.6 


+ 


2.3 


16.9 


17.5 




0.3897 


S&W 


9 








prob not var 






S&W print 


10 


- 47.8 


- 


45.6 


16.96 


17.54 


35538.528 


0.352314 S&W 


11 


- 12.2 


- 


41.9 


16.72 


17.30 


35538.670 


0.38739 S&W 


12 


+ 5.1 


- 


4.2 


16.6 


17.6 




0.5: 


S&W 


13 


+ 0.1 


- 


19.0 


16.8 


17.3 




0.3759 


S&W 


14 


+ 8.4 


- 


0.2 


16.9 


17.5 




0.5255 


Newburn 


15 


+ 9.2 


- 


7.8 


16.8 


17.3 




0.3354 


Newburn 


16 


+ 14.5 


+ 


7.7 


16.8 


17.1 




0.2775 


Newburn 


17 


+ 63.7 


+ 


143.3 


16.72 


17.34 


35538.430 


0.37473 Newburn 



Five field variables, Baade. 

Baade, AN 244.15 3 (1931); Sandage and Walker, AJ 60.230 (p) (1955); Newburn, AJ 62.197 
(1957); Mannino, Asiago Contr 87 (1958) 

S55a, S57, S59, S61, R62a, S62, L65, R65, S69 



NGC4372 a 12^23^.0, 6-72°24' 



-739.75 
+612.15 



- 42.08 
-382.25 



F&L 
F&L 



Wilkens, Letter (1961); Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966) 
S55a, 857, S59, S61, R62c, S62, F&L63, 869 

NGC 4590 (Messier 68) al2h36m.8, 6 -26° 29' 



1 


- 


283 


+ 109 


15.55 


16.11 


33421.357 


0.349604 


2 


- 


168 


- 44 


15.05 


16.29 


33661.66 


0.578169 


3 


- 


140 


+ 91 


15.40 


16.15 


33661.66 


0.4158 


4 


- 


118 


-132 


15.65 


16.20 


33423.273 


0.396367 


5 


- 


53 


+ 169 


15.47 


16.11 


33423.297 


0.282116 


6 


- 


54 


+ 17 


15.75 


16.07 


33422.413 


0.368523 


7 


- 


51 


- 78 


15.71 


16.07 


33423.478 


0.387945 


8 


- 


35 


-134 


15.74 


16.13 


33422.359 


0.390402 


9 


— 


30 


+ 40 


15.43 


16.28 


33422.257 


0.57900 


10 


- 


24 


- 14 


15.28 


16.62 


33423.224 


0.55112 


11 


- 


17 


-113 


15.65 


16.16 


33423.295 


0.36489 


12 


- 


12 


00 


15.07 


16.23 


33423.333 


0.6162 


13 


- 


4 


- 57 


15.72 


16.11 


33423.385 


0.361740 


14 


- 


2 


+ 218 


15.02 


16.25 


33421.437 


0.55679 


15 


+ 


10 


+ 59 


15.65 


16.36 


33423.360 


0.37220 


16 


+ 


10 


+ 78 


15.65 


16.22 


33423.289 


0.381967 


17 


+ 


17 


- 74 


15.65 


16.60 


33418.293 


0.66693 


18 


+ 


18 


- 96 


15.69 


16.19 


33423.327 


0.367346 


19 


+ 


32 


+ 70 


15.65 


16.20 


33421.404 


0.39206 


20 


+ 


33 


-114 


15.69 


16.14 


33421.293 


0.385764 


21 


+ 


46 


+ 8 


15.82 


16.60 


33423.358 


0.37241 


22 


+ 


61 


- 22 


15.30 


16.52 


33421.424 


0.563469 


23 


+ 


65 


+380 


14.85 


16.13 


33423.198 


0.6588799 



Catalogue 



17 



No. 


x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC 4590 (continued) 












24 


+ 72 


- 8 


15.64 


16.13 


33422.268 


0.376500 




25 


+ 140 


+ 123 


15.00 


16.15 


33423.328 


0.641556 




26 


+ 157 


- 45 


15.63 


16.11 


33799.370 


0.413217 




27 


+ 381 


+ 263 


10.2 


17.4 


33661. 


320 


FI Hya, f 


28 


+439 


+ 159 


14.81 


16.18 


33423.292 


0.6067750 




29 


+ 283 


-153 


15.65 


16.15 


33419.416 


0.395253 




30 


+ 112 


- 77 


15.60 


16.20 


33422.442 


0.73362 




31 


-109 


+ 96 


15.49 


16.10 


33423.310 


0.399658 




32 


-330 


-639 






33422.362 


0.58692 


van Agt 


33 


+ 89 


+ 59 






33422.317 


0.38523 


van Agt 


34 


+ 268 


+ 216 






33422.314 


0.39696 


van Agt 


35 


- 35 


- 52 






33421.340 


0.71608 


van Agt 


36 


- 38 


- 52 






33422.374 


0.6998 


van Agt 


37 


- 21 


+ 20 






33423.317 


0.38553 


van Agt 


38 


- 22 


- 29 






33423.251 


0.3826 


van Agt 


39 


- 50 


- 8 










T,R&0 


40 


- 1 


- 52 










T,R&0 


41 


+ 4 


+ 80 










T,R&0 


42 


- 3 


+ 37 










T,R&0 



Five new field variables, Terzan et al. (1973) 

Rosino and Pietra, Bologna Pubbl6,5 (1954); van Agt and Oosterhoff, Leiden Ann 21.25 3 (p) 
(1959); Terzan, Rutily and Ounnas, lAU Coll 21 (p) (1973) 

S55a, S57, S59, S61, R62a, L65, R65, S69 



NGC 4833 ai; 


2h56m.0, §- 


-70° 36' 










1 


-264 


+468 


15.32 


15.86 


29375.251 


0.750101 


RYMus 


2 


+ 378 


-354 


13.0 


16.2: 


26166 


333.7 


RZMus,V,f 


3 





+ 6 


15.46 


15.9 


29363.248 


0.744526 




4 





+ 24 


15.24 


15.88 


29381.249 


0.655536 




5 


+ 132 


- 66 


15.4 


16.0 


29381.240 


0.629414 




6 


+ 120 


+ 120 


15.3 


15.9 


29381.297 


0.653967 




7 


+ 72 


- 6 


15.49 


16.05: 


29374.256 


0.668422 




8 


-168 


+498 


15.59 


15.79 








9 


- 42 


6 


14.5 


15.16 


28035 


87.7: 




10 


+ 72 


+414 


15.14 


15.9 








11 


-336 


-828 


14.5 


16.0: 


24320 


303.8 




12 


+ 19.2 


+ 13.7 










F&L, RR? 


13 


+ 272.2 


- 30.2 










F&L, RR? 


14 


- 13.7 


- 38.5 










F&L, RR? 


15 


- 15.1 


- 57.7 










F&L, RR? 


16 


- 76.5 


+ 151.2 








irr 


F&L, red 



Menzies confirms variability of all these stars, with small variation for V16. He Usts eight new sus- 
pected variables, MenziesB57, 384,3105, 3121, B193, C80, C308 (all appear to be RR Lyr), and 
D199 (perhaps Pop 11 Cepheid), identified on print. 

Feast, Obs 86. 120 (1966); I'ourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966); 
Menzies, MN 156.207 (p) (1972) 

S55a, S59, R62a, S62, L65, R65. S67, S69 



18 



Variable Stars in Globular Clusters 



No. 


x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC 5024 (Messier 


53) al3hlom.5,5 


+ 18°26' 








1 


+ 9.6 


-171.0 


15.75 


17.20 


23083.408 


0.6098240 


+ 


2 


- 78.0 


-183.6 


16.30 


16.90 


22787.498 


0.3861005 




3 


- 60.6 


-138.0 


16.10 


17.10 


23113.388 


0.6306134 





4 


-169.5 


-156.6 


16.41 


16.84 


23113.482 


0.3851900 


+ 


5 


-237.0 


-258.0 


15.75 


17.10 


23143.336 


0.6394247 


- 


6 


+ 123.6 


+ 13.5 


16.00 


17.20 


23083.457 


0.66401573 


- 


7 


+ 79.5 


+ 83.5 


15.85 


17.15 


23145.418 


0.5448396 


+ 


8 


+ 72.0 


+ 60.0 


16.10 


17.10 


22762.553 


0.61553333 


- 


9 


+ 67.5 


- 40.5 


15.90 


17.10 


23145.523 


0.6003694 


- 


10 


-138.6 


+ 54.0 


15.85 


17.05 


23143.446 


0.6082562 





11 


-143.4 


- 58.5 


15.85 


17.0 


23113.525 


0.6299592 


+ 


12 


+ 409.5 


+ 187.5 


15.90 


17.15 


23113.579 


0.61258094 


- 


13 


+462.0 


-299.7 


15.75 


17.10 


23143.419 


0.6274424 


- 


14 


+ 354.6 


-207.0 


15.80 


17.10 


23143.363 


0.5454029 


- 


15 


+ 248.4 


+ 228.0 


16.39 


16.67 


23113.361 


0.3087107 


+ 


16 


-136.5 


-202.5 


16.43 


16.90 


23113.402 


0.3031728 




17 


-214.5 


+ 114.0 


16.29 


16.80 


22762.612 


0.3814992 




18 


- 96.0 


+ 12.6 


15.83 


16.42 








19 


+ 165.6 


- 42.0 


16.34 


16.85 


22789.465 


0.3918418 




20 


+ 188.4 


-351.6 


16.32 


16.81 


23113.615 


0.3844212 


- 


21 


+437.4 


- 27.0 


16.32 


16.81 


22790.410 


0.3384650 




22 


- 53.4 


-288.0 


16.56 


16.85 


var? 






23 


+ 96.0 


- 89.7 


16.34 


16.88 


23113.460 


0.3658077 




24 


-118.5 


- 29.2 


15.71 


16.43 




3.'? 




25 


+ 130.3 


+ 31.7 


16.05 


17.0 


23113.392 


0.70516256 


- 


26 


-288.0 


-279.9 


16.20 


16.85 


23113.343 


0.3911166 




27 


-203.8 


-157.9 


16.0 


17.10 


23083.620 


0.6710599 





28 


-181.4 


+459.0 


15.65 


17.05 


23113.183 


0.63279704 


+ 


29 


+ 125.4 


- 79.5 


16.56 


17.04 


22808.305 


0.8232463 


+ 


30 


+ 57.7 


-482.8 


15.6 


17.6 


31223.384 


0.53548466 


BC, 37d 


31 


+ 60.6 


- 0.1 












32 


-111.9 


- 86.6 


16.26 


16.65 


22790.475 


0.3901324 




33 


-165.0 


+ 12.2 












34 


-144.0 


-216.7 


16.48 


16.70 


not var 






35 


+ 104.1 


+ 153.2 


16.25 


16.95 


23113.327 


0.3726739 





36 


+ 120.3 


+306.5 


16.33 


16.71 


23113.698 


0.3732511 




37 


- 44.0 


+ 62.2 


15.68 


16.48 








38 


+ 21.3 


-143.2 


16.0 


17.0 


23083.773 


0.7057873 


+ 


39 


-234.0 


+ 212.5 


16.84 


17.26 


not var 






40 


+ 8.9 


+ 111.5 












41 


+ 19 


+ 66 












42 


- 67 


+ 17 


15.54 


16.33 








43 


- 34 


+ 53 












44 


+ 53 


- 2 


15.20 


15.99 








45 


- 5 


- 36 












46 


- 12 


+ 34 












47 


- 68.7 


+ 138.0 


16.20 


16.80 


37763.435 


0.35051 


Margoni 



Catalogue 



19 



No. 


X 




y" 




Max. 


Min. 


Epoch 


Period 


Remarks 


NGC 5024 (continued) 














48 


+ 


4.68 


+ 


11.58 


16.63 


17.53 


34480.91 


0.3327660 


Cuffev 47 


49 


+ 


1.05 


+ 


4.39 


15.25 


15.65 


34478.5 


111.6 


Cuffey 48 


50 


- 


2.28 


- 


1.34 


15.22 


15.52 


34482.0 


55.4 


Cuffey 49 



Cuffey, AJ 67.574 (1962); Margoni, Asiago Contr 150 (1964); Cuffey, AJ 70.732 (1965); Margoni, 
Asiago Contr 170 (1965), Bamb Kl Veroff 4.40.249 (1965): Wachmann, .Astr Abh Hoffmeister p. 
121 (1965); Cuffey, AJ 71.514 (1966); Margoni, Asiago Contr 198 (1967); Wachmann, Berg Abh 
8.114(1968) 
S55a, S57, S59, S61, R62a, S62, S64, L65, R65, S67, C&S69, S69, S70 



NGC 5053 al3hl3m.9, 6 


+ 17°57' 










1 


-380 


+ 158 


15.8 


16.5 


37343.456 


0.6471748 




2 


-193 


- 3 


15.9 


16.6 


37370.575 


0.3789561 


+ 


3 


+ 140 


+ 138 


15.8 


16.6 


37370.470 


0.5929430 




4 


+ 31 


-114 


15.8 


16.5 


37371.454 


0.6670627 




5 


+ 220 


-220 


16.0 


16.6 


37370.641 


0.7148605 




6 


+ 126 


+ 77 


16.0 


16.5 


37370.556 


0.2921978 




7 


- 87 


+ 169 


15.9 


16.5 


37370.469 


0.3519300 


+ 


8 


+ 117 


+ 50 


15.9 


16.5 


37371.452 


0.3628410 


- 


9 


-199 


+ 382 


16.0 


16.6 


37371.407 


0.7402201 




10 


+ 94 


+ 56 


16.10 


16.45 


37370.427 


0.4373803 


AltP? 


11 






16.01 


16.47 






Perova 



Perova's var., VI 1, is Baade's comparison star c. 

Perova, VS 14.255 (1962); Mannino, Bologna Pubbl 8, 12 (1963) 

S55a, S59, R62a, S62, S64, L65, R65, C&S69, S69 



NGC5139(COCentauri) al3h23m.8. 


5-47°13' 








1 


— 


416.16 


+ 298.89 


11.05 


12.45 


30027.0 


29.3479* 


0, Sp, F, V, mem 


2 


- 


340.00 


+ 238.51 


113.06 


16.12 


30139.4 


235.74 


0, f 


3 


- 


507.93 


+ 167.43 


14.11 


15.14 


27000.42 


0.8412403 


- 


4 


- 


337.61 


+ 262.10 


14.96 


15.25 


27000.32 


0.6273172 


+ 


5 


- 


282.75 


+ 328.29 


14.48 


15.49 


27000.44 


0.5152823 


+ 


6 


- 


162.43 


+ 252.95 


13.84 


15.24 


27010.1 


73.513 


0, prob f 


7 


+ 


153.19 


+879.15 


14.15 


15.33 


27000.20 


0.7130181 


+ 


8 


+ 


629.43 


+ 16.20 


14.03 


15.35 


27000.31 


0.5212859 


+ 


9 


- 


473.17 


+ 137.14 


14.31 


15.28 


30000.04 


0.5233301 





10 


- 


397.76 


+ 244.48 


14.43 


14.95 


27000.06 


0.374956 


- 


11 


- 


158.63 


+ 338.73 


13.90 


15.04 


27000.19 


0.5648246 


- 


12 


- 


193.16 


+ 274.34 


14.43 


14.95 


27000.08 


0.3867639 





13 


- 


487.26 


+ 199.54 


13.96 


15.14 


30000.50 


0.6690507 





14 


- 


473.51 


-627.56 


14.56 


15.17 


30000.29 


0.3771102 





15 


- 


194.09 


+ 242.62 


13.70 


14.39 


27000.40 


0.8106152 


+ 


16 


+ 


517.05 


-536.81 


14.46 


15.04 


27000.07 


0.3301802 


+ 


17 


+ 


522.24 


+ 200.00 


14.18 


14.61 


30062.2 


64.725 


irr, prob f 


18 


+ 


596.64 


+ 220.15 


14.06 


15.35 


30000.42 


0.6216671 






20 



Variable Stars in Globular Clusters 



No. 




x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC5139 (continued) 












19 


+ 


444.14 


+ 32.44 


14.76 


15.30 


30000.11 


0.2995525 





20 


+ 


280.88 


+ 32.06 


14.09 


15.28 


27000.61 


0.6155528 


+ 


21 


- 


355.75 


+ 162.07 


14.20 


14.81 


30000.10 


0.380810 




22 


+ 


552.18 


-330.22 


14.63 


15.17 


27000.22 


0.3965212 




23 


+ 


2.54 


+ 240.71 


14.26 


15.39 


27000.17 


0.5108653 


+ 


24 


+ 


524.71 


-336.96 


14.57 


15.04 


27000.08 


0.4622076 


+ 


25 


- 


210.77 


+ 17.48 


13.98 


15.07 


30000.50 


0.5885146 





26 


- 


229.58 


+ 101.21 


14.36 


15.06 


27000.15 


0.7847138 


+ 


27 


- 


205.47 


+ 24.11 


14.50 


15.19 


30000.02 


0.6157067 





28 








not var 










29 


- 


193.25 


- 6.45 


12.39 


13.50 


30008.98 


14.73383 


0, Cep, mem 


30 


- 


307.92 


- 75.01 






30000.21 


0.403988 





31 








not var 










32 


+ 


174.39 


+420.01 


13.87 


15.20 


27000.39 


0.6204298 


- 


33 


- 


554.54 


- 24.00 


14.16: 


15.25: 


27000.52 


0.6023334 


- 


34 


- 


396.87 


-269.04 


14.10: 


15.00:: 


27000.55 


0.7339428 


+ 


35 


+ 


71.70 


+ 365.07 


14.43 


15.00 


27000.00 


0.3868382 


- 


36 


+ 


246.11 


+789.42 


14.62 


15.17 


30000.26 


0.379846 





37 








not var 










38 


+ 


169.10 


-470.37 


14.45 


15.20 


27000.01 


0.7790474 


+ 


39 


+ 


741.86 


-365.80 


14.48 


15.08 


30000.21 


0.3933505 





40 


- 


220.99 


-125.30 


13.95 


15.15 


30000.11 


0.6340925 





41 


+ 


151.80 


-142.18 


14.03 


15.06 


27000.53 


0.6629590 


+ 


42 


+ 


0.21 


- 50.21 


12.5 


14.9 




149.4 




43 


+ 


119.23 


+ 103.16 


13.27 


14.29 


30000.65 


1.156706 


0, Cep, mem 


44 


- 


243.40 


-354.05 


13.67: 


14.65: 


30000.48 


0.5675440 





45 


- 


764.48 


+ 80.97 


14.18 


15.37 


27000.09 


0.5891301 


+ 


46 


- 


770.61 


+ 170.11 


14.43 


15.44 


27000.60 


0.6869406 


+ 


47 


- 


504.32 


+ 269.26 


14.07 


14.60 


27000.15 


0.4851319 


- 


48 


- 


86.54 


-104.54 


12.95 


13.80 


30003.6 


4.47227 


0, Cep, mem 


49 


- 


391.98 


-553.77 


14.40 


15.52 


30000.36 


0.6046505 





50 


- 


530.75 


+ 65.40 


14.32 


14.90 


30000.20 


0.3861960 





51 


— 


36.85 


+258.73 


13.86 


15.16 


27000.08 


0.5741332 


+ 


52 


- 


112.85 


+ 36.47 


13.60 


14.22 


30000.28 


0.6603703 





53 


— 


482.79 


-447.74 


13.30 


13.87 




32.7 


irr, Alt 70 


54 


- 


229.39 


+592.76 


14.33 


15.22 


27000.30 


0.7728973 


+ 


55 


- 


617.73 


-816.68 


14.50 


15.50 


27000.11 


0.5817244 


- 


56 


- 


515.93 


-541.96 


14.56 


15.57 


27000.42 


0.5680098 


- 


57 


+ 


635.72 


-493.26 


14.52 


15.16 


27000.44 


0.7944181 


+ 


58 


- 


335.44 


+277.68 


14.49 


14.74 


30000.28 


0.3699124 





59 


- 


282.90 


- 65.84 


14.20 


15.18 


30000.41 


0.5185122 





60 


- 


108.42 


-247.33 


13.24 


14.47 


30001.00 


1.349464 


0, Cep, mem 


61 


+ 


280.44 


+ 68.07 


13.65 


14.42 


30001.59 


2.273564 


0, Cep, mem 


62 


— 


199.80 


+ 45.28 


13.88 


15.10 


27000.31 


0.6197945 


+ 


63 


- 


996.82 


-491.46 


14.59 


15.17 


27000.24 


0.8259432 


+ 


64 


- 


448.01 


-457.49 


14.54 


15.14 


30000.24 


0.344621 


+ 


65 


- 


454.49 


-474.32 


14.72: 


15.17: 


30000.022 


0.06272267 


0, f, RRs 



Catalogue 



21 



No. 




x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC5139 (continued) 












66 


_ 


133.37 


+ 375.15 


14.46 


14.95 


27000.24 


0.4074106 


+ 


67 


- 


178.11 


+593.57 


14.18 


15.28 


27000.41 


0.5644510 


+ 


68 


- 


338.18 


+545.12 


14.15 


14.67 


30000.1 


0.534708 





69 


- 


965.76 


+530.94 


14.14 


15.35 


27000.24 


0.6532208 


+ 


70 


+ 


417.83 


-304.65 


14.62 


15.11 


30000.2 


0.390596 





71 


+ 


220.39 


+ 47.13 


14.38 


14.92 


30000.2 


0.3574826 





72 


+ 


477.85 


+ 734.87 


14.44 


15.10 


27000.17 


0.3845221 


+ 


73 


- 


532.49 


+750.76 


14.00 


15.32 


27000.42 


0.5752151 


+ 


74 


+ 


215.47 


+664.83 


14.10: 


15.29: 


27000.43 


0.5032480 


+ 


75 


+ 


341.44 


+ 591.55 


14.52 


15.07 


30000.16 


0.4283681 





76 


+ 


113.31 


+511.81 


14.21: 


14.72: 


27000.17 


0.3378487 


+ 


77 


+ 


352.29 


+ 392.42 


14.39 


14.85 


30000.10 


0.4260045 





78 


+ 


586.10 


+ 146.68 


14.17 


14.84 


33929.972 


1.16812901 


-,EA,Min,mem 


79 


+; 


1000.12 


- 51.02 


14.26 


15.39 


27000.23 


0.6082758 


+ 


80 


+j 


1304: 


-108: 


14.1: 


14.8 




0.45 


Alt 0.31 


81 


+ 


511.36 


+ 228.72 


14.39 


14.93 


27000.14 


0.3894005 


+ 


82 


+ 


499.94 


+ 126.98 


14.47 


15.00 


30000.12 


0.335931 





83 


+ 


226.09 


+424.66 


14.50 


15.07 


27000.29 


0.3566071 


+ 


84 


-: 


1202.81 


- 74.70 


14.37: 


15.10: 


30000.33 


0.5798732 





85 


-] 


1010.51 


+ 307.98 


14.33 


15.13: 


27000.10 


0.7427583 


+ 


86 


+ 


293.14 


+ 147.26 


13.96 


15.18 


27000.32 


0.6478337 


+ 


87 


+ 


113.68 


+ 184.13 


14.40 


14.90 


30000.04 


0.3965978 





88 


+ 


98.13 


+ 203.28 


14.01 


14.81 


27000.22 


0.6901959 


+ 


89 


- 


2.95 


+ 159.29 


14.47 


14.97 


30000.29 


0.374948 





90 


- 


5.30 


+ 137.09 


13.81 


14.73 


27000.48 


0.6034020 


+ 


91 


+ 


43.72 


+ 144.35 


14.25 


14.91 


27000.18 


0.8951197 




92 


- 


317.86 


+446.38 


14.10: 


14.68: 


30000.00 


1.345044 


0, Cap, mem 


93 








not var 










94 


- 


504.09 


+355.09 


14.58: 


14.99: 


30000.20 


0.2539334 





95 


- 


824.80 


- 11.05 


14.51 


15.02 


27000.39 


0.4050201 


+ 


96 


- 


71.20 


+ 97.06 


13.93 


14.82 


27000.08 


0.6245320 


+ 


97 


+ 


225.50 


+ 187.93 


14.11 


15.16 


27000.65 


0.6918907 


+ 


98 


+ 


198.25 


+ 102.38 


14.57 


15.09 


30000.19 


0.2805649 





99 


+ 


160.35 


+ 50.36 


13.77 


14.90 


37000.59 


0.766140 


+ 


100 


+ 


179.49 


+ 65.68 


14.05 


15.05 


27000.48 


0.5527119 


+ 


101 


+ 


444.11 


- 73.28 


14.46 


14.90 


26523.291 


0.3408843 




102 


+ 


361.83 


- 94.10 


14.16 


15.22 


27000.13 


0.6913899 


+ 


103 


+ 


283.14 


+ 2.35 


14.46 


14.80 


30000.02 


0.3288489 





104 


+ 


822.98 


-309.01 


14.52 


14.94 


37000.51 


0.867280 


- 


105 


+ 


603.23 


-246.92 


14.70 


15.25 


27000.14 


0.3353345 


+ 


106 


+ 


130.35 


+ 26.92 


13.88 


15.02 


27000.22 


0.5699061 


- 


107 


+ 


279.83 


-139.13 


14.07 


15.39 


27000.07 


0.5141002 


+ 


108 


+ 


185.66 


- 46.36 


13.84 


14.81 


27000.24 


0.5944554 


+ 


109 


+ 


153.91 


- 57.13 


13.99 


15.03 


27000.67 


0.7440615 


+ 


110 


+ 


158.94 


- 87.08 


14.41 


14.96 


26524.256 


0.3221021 




111 


+ 


27.26 


- 0.30 


14.18 


14.80 


27000.02 


0.7629005 


+ 


112 


+ 


79.83 


-103.36 


13.92 


14.92 


30000.07 


0.4743558 






22 



Variable Stars in Globular Clusters 



No. 




x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC5139 (continued) 












113 


+ 


99.99 


-187.65 


13.94 


15.22 


27000.39 


0.5733636 


+ 


114 


+ 


38.08 


-101.15 


14.00 


14.75 


26470.416 


0.6753065 




115 


— 


345.49 


-336.14 


14.12 


15.30 


27000.14 


0.6304638 


- 


116 


- 


109.66 


+ 33.71 


14.12 


14.77 


30000.37 


0.7201327 





117 


— 


267.73 


- 40.22 


14.40 


14.92 


30000.17 


0.4216616 





118 


- 


58.87 


- 98.67 


13.88 


15.02 


30000.03 


0.6116283 





119 


— 


82.04 


-157.45 


14.51 


14.83 


26472.319 


0.3058774 




120 


- 


211.29 


-247.61 


14.26 


15.23 


27000.51 


0.5485746 


- 


121 


_ 


184.36 


-189.58 


14.48 


14.81 


27000.00 


0.3041811 


+ 


122 


- 


162.92 


-261.41 


13.99 


15.17 


27000.06 


0.6349267 


+ 


123 


+ 


46.11 


-512.55 


14.42 


14.91 


26473.331 


0.4739051 




124 


+ 


78.88 


-626.81 


14.37 


14.97 


30000.02 


0.3318607 





125 


+ 


23.74 


-742.59 


14.04 


15.33 


27000.26 


0.5928884 


+ 


126 


+ 


822.95 


-730.44 


14.45 


14.97 


30000.17 


0.3418905 





127 


- 


880.16 


+ 4.31 


14.60 


15.12 


30000.03 


0.3052736 





128 


- 


289.77 


- 92.09 


14.25 


14.86 


27000.43 


0.8349478 


+ 


129 


+ 


192.02 


- 25.83 


14.18 


14.74 






f 


130 


- 


366.17 


+900.99 


14.13 


15.49 


30000.38 


0.4932499 





131 


— 


165.05 


- 59.95 


14.40 


14.86 


27000.19 


0.3921558 


- 


132 


- 


72.44 


- 29.31 


13.97 


14.96 


26469.386 


0.6556410 




133 


- 


1914.22 


+ 1053.78 


13.74 


14.53 


30000.07 


0.31709593 


0,EW, Min 


134 


- 


942.87 


+ 972.72 


14.12 


15.32 


30000.57 


0.6529026 





135 


- 


184.88 


- 37.25 


13.87 


14.85 


26470.314 


0.6325795 




136 


- 


154.26 


+ 60.08 


14.22 


14.64 


30000.0 


0.3919136 





137 


- 


149.54 


+ 96.23 


14.38 


14.90 


30000.29 


0.3342179 





138 


- 


111.12 


- 187.55 


12.5 


13.6 




74.6: irr. 




139 


- 


86.94 


+ 65.18 


14.00 


14.90 


26462.404 


0.6768666 




140 


- 


42.65 


- 86.80 








short 




141 


- 


55.47 


- 47.46 


14.05 


14.75 


irr 


0.6975651 




142 


- 


37.35 


2.56 


14.2 


14.8 




short 




143 


- 


37.45 


+ 71.40 


14.24 


14.77 


26470.394 


0.8207020 




144 


- 


33.28 


+ 22.44 


14.33 


14.81 


26454.329 


0.8353054 




145 


+ 


49.07 


- 148.51 


14.40 


14.87 


30000.15 


0.373139 





146 


+ 


65.96 


- 48.03 


13.87 


14.77 


26469.386 


0.6331021 




147 


+ 


298.70 


- 151.04 


14.35 


14.80 


30000.34 


0.4226989 





148 


+ 


299.20 


+ 44.21 


12.9 


13.8 




90: irr. 




149 


+ 


477.33 


+ 894.18 


14.03 


15.11 


30000.42 


0.6827281 





150 


+ 


543.18 


- 442.23 


14.07 


14.94 


30000.7 


0.8991997 





151 


+: 


1010.06 


+ 753.35 


14.42 


14.84 


30000.1 


0.4077838 





152 


+ 


13.84 


- 48.83 


12.8 


13.7 




124: 


irr 


153 


+ 


34.46 


+ 136.32 


14.48 


14.88 


30000.23 


0.386445 





154 


+ 


169.59 


- 113.20 


14.55 


14.72 


30000.10 


0.322407 





155 


+ 


75.25 


+ 237.31 


14.43 


14.88 


30000.3 


0.413919 





156 


+ 


15.06 


- 191.94 


14.41 


14.83 


30000.34 


0.3591887 





157 


+ 


1.77 


+ 82.58 


14.42 


14.79 


26523.370 


0.4064970 




158 


- 


10.58 


- 119.80 


14.32 


14.74 


26472.442 


0.3673350 




159 


-; 


2039.94 


- 891.45 


14.39 


14.96 


30000.0 


0.343101 






Catalogue 



23 



No. 


x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC5139 (contii 


lued) 












160 


- 711.13 


+ 969.21 


14.51 


15.15 


30000.1 


0.397276 





161 


- 96.81 


- 129.27 


13.3 


13.8 




irr 




162 


- 392.40 


- 252.39 


12.9 


13.6 




irr 


est now 


163 


- 575.24 


+ 499.91 


14.59 


14.88 


30000.0 


0.3132294 





164 


+ 152.75 


+ 478.38 


13.7 


14.0 




37: t 


Red 


165 


- 69.92 


+ 104.59 












166 


2.89 


+ 144.71 












167 


- 352.63 


- 321.43 












168 


- 543.66 


-. 201.42 


14.96 


15.46 


30000.1 


0.321295 





169 


+ 347.5 


+ 278.7 


14.61 


14.85 


32323.35 


0.46926 


Belserene 


170 












irr 


Eggen, Herst53 


171 


-2280 


+ 2520 








RRa 


Wilkens 1 


172 


+ 720 


+ 1440 








RRa 


Wilkens 2 


173 


+ 1800 


+ 660 








RRa 


Wilkens 3 


174 


+ 780 


-2040 








1.8984 


Wilkens 4, E 


175 


-2640 


-3000 










Wilkens 5 


176 


+ 144 


- 66 








RRc 


Wilkens 6 


177 


+ 1380 


- 480 








RRb 


Wilkens 7 


178 


+ 3120 


+ 600 








RRb 


Wilkens 8 


179 


-1800 


-2940 








RRb 


Wilkens 9 


180 


-1500 


- 720 








RRc 


Wilkens 10 


181 


+ 1925 


-1216 








0.58836 


Wess2 


182 


+ 3355 


+ 1292 








0.54539 


Wess 12 


183 


+ 1744 


- 116 








0.29605 


Wess 13 



* This variable appears intermediate between W Vir and RV Tau types, with alternate P 58<^.7. 
t Period from Dickens (1972). 

Wilkens now considers his vars. 1, 5, 8, 9 also members (Letter, 1972), nos. 1 1-15 suspected. 
Wesselink has one field EW. 

Belserene, Rutherfurd Contr 33.1,43 (1956), AJ 64.58 (1959); Thackeray, Obs 80.226 (1960); 
Eggen, Royal Obs Bull 29.E73 (1961); Kurochkin, VS 13.248 (1961); Belserene, AJ 69.475 (1964); 
Dickens and Saunders, Royal Obs Bull lOl.ElOl (1965); Geyer, AG Mitt p. 96 (1965); Geyer and 
Szeidl, Bamb Kl Veroff 4, 40.63 (1965); Harding, Royal Obs Bull 99.E65 (1965); Wilkens, MVS 
3.72 (1965); Oosterhoff and Wahaven, BAN 18.387 (1966); Ponsen and Oosterhoff, BAN Suppl 
1.3 (1966); Woolley, Royal Obs Ann 2 (1966); Dickens and Carey, Royal Obs Bull 129 (1967); 
Geyer, ZAp 66.16 (1967); Wilkens, MVS 4.93 (1967); Jones, MN 140.265 (1968); Sistero, IBVS 
316 (1968); Wilkens, La Plata Bol 12 (1968); van Albada, AAS Bull 1.366 (1969); Sistero, Four- 
cade and Laborde, IBVS 402 (1969): Wesselink, Letter (1969); Geyer and Szeidl, Astr and Ap 4.40 
(1970); Geyer, lAU Coll 15.235 (1971); Dickens, Letter (1972); Dickens, Feast and Lloyd Evans, 
MN 159.337(1972); Eggen, ApJ 172.639 (1972); Feast, Preprint (1972); Geyer, AG Mitt 31.168 
(1972); Wesselink, unpub (1972); Wilkens, Letter (1972) 

S55a, S57, S59, S61, A62, R62a, S62, P64, S64, L65, R65, FLA66, St66, S67, C&S69, S69, S70 



NGC 5272 (Messier 3) a 13h39m.9, 6 +28°38' 

14.68 15.92 



1 - 5.2 - 128.5 

2 + 15.8 + 52.6 

3 + 57.9 - 66.0 



14.75 16.00 



36692.336 
15021.225 



0.5206250 
0.5582053 



24 



Variable Stars in Globular Clusters 



No. 




x" 




y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC5272 (continued) 












4 


— 


43.5 


— 


8.8 


14.9 


16.0 








5 


+ 


261.0 


- 


22.3 


14.71 


16.15 


15021.239 


0.5058940 


BC 


6 


- 


123.9 


+ 


60.1 


14.87 


16.21 


36669.320 


0.5143228 


+ 


7 


- 


4.8 


+ 


87.2 


14.69 


16.25 


15021.064 


0.4974290 




8 


- 


81.7 


- 


23.4 


14.37 


15.4 






Confirmed 


9 


- 


291.4 


- 


207.8 


14.95 


16.28 


36668.502 


0.5415641 


- 


10 


+ 


153.6 


+ 


138.0 


15.06 


16.15 


36658.470 


0.5695185 


- 


11 


- 


152.6 


- 


209.7 


14.75 


16.17 


36699.491 


0.5078918 


est 


12 


- 


3.8 


- 


145.4 


15.23 


15.83 


36687.336 


0.3178890 




13 


- 


26.0 


- 


137.5 


14.79 


15.96 


36702.398 


0.4830302 


- RR Binary? 


14 


- 


49.0 


- 


161.0 


14.95 


16.19 


36668.549 


0.6359019 


+ 


15 


- 


90.8 


- 


273.2 


14.87 


16.26 


36666.565 


0.5300794 


+ 


16 


- 


301.4 


- 


93.1 


14.93 


16.31 


36687.369 


0.5115075 


- 


17 


+ 


142.4 


- 


440.4 


15.20 


16.20 


36668.543 


0.5761417 


+, B2 


18 


+ 


97.6 


- 


295.3 


14.86 


16.30 


36661.578 


0.5163623 


Be 


19 


+ 


350.5 


- 


245.6 


15.56 


16.15 


36639.520 


0.6319796 


- 


20 


+ 


333.5 


- 


271.6 


14.85 


16.25 


36668.555 


0.4912411 




21 


+ 


346.9 


+ 


17.9 


14.81 


16.27 


30000.415 


0.5157336 


+ 


22 


+ 


190.2 


- 


10.7 


14.98 


16.20 


36660.5 36 


0.4814208 




23 


- 


113.0 


+ 


279.2 


15.07 


15.80 


15021.082 


0.5953756 




24 


- 


147.6 


+ 


10.4 


15.06 


16.07 


15021.563 


0.6633494 


est 


25 


- 


124.4 


- 


31.4 


14.66 


16.07 


15021.089 


0.4800510 


+ 


26 


— 


177.4 


- 


43.0 


14.88 


16.04 


15021.239 


0.5977452 


- 


27 


- 


110.2 


- 


102.8 


15.07 


16.11 


15021.566 


0.5790912 




28 


- 


25.0 


- 


105.8 


14.92 


15.88 


24290.335 


0.4706364 




29 


- 


65.2 


- 


73.6 












30 


- 


36.5 


+ 


58.0 


15.18 


15.92 


22760.635 


0.5120902 




31 


+ 


33.1 


+ 


65.1 


14.43 


15.65 


15021.542 


0.5807216 


- 


32 


+ 


11.8 


+ 


60.1 


14.58 


15.68 


15021.108 


0.4953518 


- 


33 


+ 


70.5 


- 


89.1 


14.78 


15.90 


15021.217 


0.5252237 


-,Be 


34 


+ 


135.4 


+ 


170.2 


15.08 


16.16 


36668.467 


0.5591012 


Be 


35 


- 


107.3 


- 


278.2 


15.04 


16.10 


15021.032 


0.5306059 


Be 


36 


+ 


172.0 


- 


35.4 


14.78 


16.26 


36692.5 25 


0.5455855 


+ 


37 


- 


236.7 


+ 


164.7 


15.34 


16.12 


30000.241 


0.3266384 


- 


38 


- 


203.0 


+ 


127.7 


14.74 


16.16 


24290.304 


0.5580276 


-,BC 


39 


- 


243.6 


+ 


121.4 


15.14 


16.23 


15021.073 


0.5870766 


Be 


40 


- 


271.2 


+ 


112.4 


15.01 


16.32 


30000.397 


0.5515416 




41 


- 


93.3 


+ 


54.0 


15.22 


16.23 


15021.441 


0.4850462 




42 


- 


78.6 


+ 


41.0 


14.40 


15.68 


15021.515 


0.5901852 




43 


+ 


99.9 


+ 


24.7 


14.40 


15.80 


15021.191 


0.5405790 


Be 


44 


+ 


170.0 


+ 


99.4 


14.84 


16.04 


15021.368 


0.5063961 


Be 


45 


- 


241.2 


- 


129.9 


14.94 


16.23 


15021.349 


0.5368966 




46 


- 


128.1 


- 


51.5 


15.32 


15.96 


15021.264 


0.6133669 




47 


- 


117.5 


- 


73.2 


14.74 


15.97 


15021.459 


0.5409923 


Be 


48 


+ 


126.9 


- 


102.7 


15.23 


15.92 


36669.346 


0.6278128 




49 


+ 


140.0 


- 


100.7 


14.71 


16.11 


36715.388 


0.5482196 


Be 


50 


+ 


8.8 


- 


234.0 


14.57 


16.09 


36669.560 


0.5130879 


Be 


51 


+ 


30.8 


- 


226.4 


15.16 


16.18 


36702.392 


0.5839818 





Catalogue 



25 



No. 




x" 




y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC5272 (cont 


nue 


d) 












52 


- 


76.8 


+ 


152.0 


14.92 


16.06 


15021.485 


0.5162250 


Be 


53 


- 


7.4 


+ 


122.8 


14.68 


15.93 


15021.006 


0.5048878 




54 


- 


32.6 


+ 


106.4 


14.92 


15.94 


15021.193 


0.5063150 




55 


- 


204.2 


+ 


324.4 


14.88 


16.31 


30000.032 


0.5298136 




56 


- 


141.1 


+ 


358.6 


15.38 


16.02 


22760.623 


0.3295986 




57 


+ 


155.2 


- 


0.2 


14.84 


16.23 


15021.618 


0.5122223 




58 


- 


86.2 


+ 


Ad.l 


14.58 


15.91 


22760.621 


0.5170617 




59 


- 


109.8 


- 


228.4 


15.23 


16.20 


36699.425 


0.5888053 




60 


- 


297.8 


- 


315.4 


15.24 


16.15 


15021.389 


0.7077228 




61 


+ 


190.2 


+ 


363.0 


14.96 


16.21 


15021.076 


0.5209312 


BC 


62 


+ 


90.2 


+ 


417.0 


15.42 


16.16 


15021.331 


0.6524077 




63 


+ 


37.2 


+ 


341.9 


14.96 


16.22 


15021.094 


0.5704164 


BC 


64 


+ 


114.8 


+ 


330.4 


15.32 


16.26 


30000.382 


0.6054590 




65 


+ 


125.4 


+ 


327.5 


14.79 


16.22 


30000.332 


0.6683394 




66 


- 


101.4 


+ 


121.4 


15.20 


15.93 


15021.323 


0.6201827 




67 


- 


131.4 


+ 


123.0 


14.95 


16.07 


15021.411 


0.5683609 


B2 


68 


+ 


21.9 


+ 


174.8 


15.0 


16.0 




0.3559732 


BC 


69 


+ 


80.6 


+ 


141.0 


15.15 


16.05 


36692.851: 


0.5665878 




70 


+ 


37.6 


+ 


152.2 


15.22 


15.75 


15021.315 


0.486: 


BC 


71 


+ 


160.6 


- 


2.0 


15.07 


16.04 


15021.168 


0.5490517 




72 


f 


445.5 


- 


2.2 


14.80 


16.30 


15021.327 


0.4560739 




73 


+ 


438.5 


+ 


62.2 


15.0 


16.0 








74 


+ 


88.2 


+ 


151.0 


14.80 


16.20 


36668.389 


0.4921441 




75 


+ 


49.0 


+ 


159.5 


15.38 


15.98 


36668.411 


0.3140790 




76 


- 


14.4 


- 


88.2 


14.90 


16.46 


15021.293 


0.5017544 




77 


- 


94.4 


+ 


27.8 


14.63 


16.07 


15021.451 


0.4593425 




78 


+ 


47.5 


+ 


66.4 


14.92 


15.70 


15021.249 


0.6119254 




79 


+ 


43.4 


+ 


349.4 


14.72 


16.31 


15021.229 


0.4833275 


BC 


80 


+ 


416.8 


+ 


284.6 


14.80 


16.17 


15021.433 


0.5384827 


BC 


81 


+ 


342.8 


+ 


351.1 


14.86 


16.30 


30000.461 


0.5291108 




82 


- 


102.6 


- 


601.8 


14.96 


16.31 


36668.477 


0.5245061 




83 


- 


441.6 


+ 


113.4 


14.87 


16.32 


15021.046 


0.5012408 




84 


+ 


64.0 


+ 


165.2 


15.26 


16.12 


36666.463 


0.5957289 




85 


+ 


306.2 


4 


225.8 


15.32 


15.92 


22760.517 


0.3558189 




86 


+ 


513.0 


- 


114.2 


15.42 


16.06 


15021.016 


0.2926601 




87 


+ 


110.6 


+ 


60.2 


15.13 


15.68 


22760.535 


0.3574814 




88 




35.0 


- 


70.2 


15.08 


15.67 


24290.324 


0.2985092 




89 


+ 


28.0 


- 


110.8 


14.85 


15.93 


15021.507 


0.5484779 




90 


+ 


97.2 


- 


188.2 


14.92 


16.25 


36692.397 


0.5170334 




91 




14.3 




550.0 


14.95 


16.26 


36669.366 


0.5301630 




92 


- 


29.0 


- 


408.4 


14.94 


16.30 


15021.083 


0.5035553 




93 


- 


319.4 


- 


396.6 


15.24 


16.27 


30000.420 


0.6023007 




94 


- 


488.4 


- 


224.6 


14.90 


16.33 


30000.304 


0.5236936 




95 




154.7 


+ 


15.4 


13.73 


14.42 




103.19 




96 


- 


164.2 


- 


234.0 


14.74 


16.10 


36692.470 


0.4994467 




97 


- 


130.0 


- 


196.7 


15.53 


16.04 


" 61.581 


0.33492C9 




98 


+ 


132.4 


- 


3.2 


not var 










99 


+ 


201.8 




55.0 


14.8 


15.8 









26 



Variable Stars in Globular Clusters 



No. 




x" 




y" 


Max. 


Min. 


Epoch 


Period Remarks 


NGC5272 (continued) 










100 


+ 


69.9 


+ 


97.3 


15.31 


15.96 




0.6188126 


101 


+ 


46.4 


+ 


83.7 


15.29 


15.78 


15021.101 


0.6438975 


102 


+ 


58.4 


+ 


114.9 


15.2 


15.9 


varV 




103 


+ 


58.1 


+ 


120.4 


not var 








104 


- 


25.8 


+ 


145.5 


14.73 


15.99 


15021.288 


0.5699231 


105 


- 


20.9 


+ 


191.6 


15.33 


15.72 


36668.548 


0.2877427 


106 


- 


48.0 


+ 


168.0 


15.18 


16.04 


36666.372 


0.5471593 


107 


- 


75.8 


+ 


335.0 


15.40 


16.14 


30000.039 


0.3090348 


108 


- 


219.0 


+ 


310.9 


14.94 


16.30 


30000.250 


0.5196047 


109 


- 


89.3 


+ 


2.7 


14.56 


15.64 


15021.033 


0.5339239 


110 


- 


99.4 


- 


15.8 


15.02 


15.88 


15021.397 


0.5353569 


111 


- 


92.7 


+ 


21.9 


15.06 


16.02 


15021.402 


0.5102469 BC 


112 


- 


144.6 


- 


719.4 


not var 








113 


+ 


199.8 


- 


689.8 


14.90 


16.25 


15021.241 


0.5130066 


114 


+ 


11.8 


+ 


622.0 


15.18 


16.24 


15021.515 


0.5977270 


115 


+ 


445.0 


+ 


664.7 


14.98 


16.34 


15021.297 


0.5133529 


116 


- 


491.8 


+ 


465.2 


14.89 


16.32 


15021.441 


0.5148088 


117 


+ 


89.6 


- 


467.6 


15.22 


16.22 


15021.579 


0.6005164 


118 


+ 


144.4 


- 


292.2 


14.90 


16.36 


15021.272 


0.4993807 


119 


+ 


253.4 


+ 


106.2 


14.76 


16.25 


30000.192 


0.5177411 


120 


- 


295.8 


+ 


231.4 


15.56 


16.07 


15021.284 


0.6401387 


121 


- 


43.6 


+ 


56.1 


14.84 


15.54 


22760.550 


0.5351882 


122 


- 


33.5 


- 


46.4 


14.6 


16.1 




0.5017 


123 


- 


259 


- 


985 


14.92 


16.31 


15021.395 


0.5454472 


124 


- 


66.4 


- 


201.4 


15.50 


15.96 


36685.349 


0.7524328 


125 


+ 


186.3 


- 


132.8 


15.48 


16.00 


36666.585 


0.3498206 


126 


- 


15.4 


- 


146.4 


15.42 


15.96 


15021.208 


0.3484043 


127 


+ 


95.6 


- 


63.6 


not var 








128 


+ 


114.6 


+ 


131.4 


15.40 


15.86 




0.2922710 Be 


129 


- 


43.6 


+ 


77.2 


15.2 


16.1 




0.305471 


130 


+ 


4.2 


+ 


84.6 


15.27 


16.00 


22760.347 


0.5688172 Be 


131 


- 


73.2 


+ 


27.4 


15.04 


15.56 


15021.318 


0.2976919 


132 


- 


53.6 


- 


22.0 


15.3 


16.4 


24290.387 


0.3398479 


133 


- 


58.6 


+ 


43.5 


14.89 


15.96 


15021.482 


0.5507230 


134 


- 


22.4 


+ 


5 2.4 


14.9 


16.3 


24290.282 


0.6190 


135 


- 


27.0 


+ 


38.0 


15.0 


16.5 




0.56843 


136 


- 


25.4 


+ 


33.4 


15.6 


16.2 






137 


+ 


53.0 


- 


18.8 


15.30 


16.04 


15021.155 


0.5751464 


138 


- 


263.6 


+ 


41.9 


14.0 


14.46 


35608.96 


80.98 


139 


+ 


34.5 


+ 


28.0 


15.25 


16.12 


22760.465 


0.560004 


140 


- 


15.7 


+ 


108.9 


15.07 


15.51 


22760.216 


0.3331304 


141 


-1497.5 


- 


249.9 


14.98 


15.97 




0.2695671 RVCVn, EW,f 


142 


- 


30 


- 


59 


14.79 


15.72 


24290.397 


0.5686256 


143 


- 


34 


+ 


16 


15.4 


16.4 


24290.337 


0.51111 


144 


+ 


54 


- 


100 


15.27 


15.99 


24290.565 


0.5967843 


145 


+ 


29 


+ 


8 


14.9 


16.5 


24290.528 


0.514456 


146 


+ 


96 


- 


59 


14.6 


16.5 


24290.563 


0.596740 


147 


- 


21 


+ 


46 


15.1 


16.3 


24290.005 


0.34644 



Catalogue 



27 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC5272 (continued) 



148 


- 


7 


+ 


37 


15.3 


16.4 


24290.170 


0.467246 


149 


+ 


34 


+ 


52 


14.7 


16.5 


24290.228 


0.54985 


150 


+ 


69 


+ 


37 


14.8 


16.7 


24290.359 


0.52397 


151 


+ 


4 


- 


40 


14.9 


16.3 


24290.191 


0.51705 


152 


+ 


77 


+ 


50 


15.42 


15.76 


24290.355 


0.3261217 


153 


- 


38 


+ 


60 


not var 








154 


+ 


2 


- 


29 


12.1 


13.7 


38873.53 


15.290 


155 


- 


64 


- 


74 










156 


- 


21 


-^ 


42 


15.0 


15.9 


38872.331 


0.531979 


157 


- 


17 


+ 


35 


14.2 


15.7 


24647.650: 


0.5283 


158 


- 


16 


- 


41 


15.2 


16.5 


24647.564: 


0.50809? 


159 


- 


15 


+ 


16 


14.9 


16.6 


24647.602: 


0.5337 


160 


- 


9 


^ 


44 


14.9 


16.1 


24647.446 


0.64792 


161 


+ 


17 


- 


58 


15.4 


16.4 


24647.567: 


0.49874 


162 


+ 


28 


- 


32 


not var 








163 


- 


16 


- 


32 


not var 








164 


+ 


21 


- 


36 


15.3 


15.9 






165 


+ 


73 


- 


20 


14.7 


16.5 


24647.544 


0.483638 


166 


- 


97 


- 


8 


15.4 


16.1 


38867.364 


0.485622 


167 


- 


78 


- 


37 


15.62 


16.00 


24647.448 


0.6439839 


168 


- 


45 


+ 


7 


14.9 


16.0 


24647.617 


0.3770 


169 


- 


29 


- 


35 


not var 








170 


- 


28 


+ 


32 


15.1 


16.1 


24647.716: 


0.43725 


171 


- 


27 


+ 


16 


15.0 


16.1 


24647.864 


0.4303 


172 


- 


21 


+ 


25 


14.9 


16.5 


24647.700 


0.59400 


173 


- 


13 


+ 


39 


15.2 


16.6 


24647.670: 


0.606990 


174 


- 


9 


- 


34 


15.1 


16.1 


24647.710 


0.4082 


175 


+ 


42 


+ 


26 


14.9 


16.2 


24647.914 


0.60780 


176 


+ 


46 


+ 


32 


14.8 


16.4 


24647.621 


0.55599 


177 


+ 


63 


- 


29 


15.52 


15.90 


24647.953 


0.3483438 


178 


+ 


79 


+ 


46 


15.51 


15.81 


24647.755 


0.2650805 


179 


+ 


39 


- 


774 


not var 








180 


- 


19 


- 


27 


not var 








181 


- 


30 


- 


14 


not var 








182 


- 


19 


+ 


60 


not var 








183 


+ 


29 


+ 


7 


not var 








184 


- 


25 


- 


14 


14.9 


16.4 


24647.841 


0.517 


185 


- 


15 


+ 


32 


15.2 


16.1 






186 


+ 


12 


- 


64 


15.1 


16.1 


24647.670 


0.675 


187 


- 


23 


+ 


9 


14.9 


16.2 


24647.961 


0.3927 


188 


- 


27 


+ 


24 


15.0 


16.0 


24647.615: 


0.3677 


189 


- 


25 


- 


21 


15.2 


16.0 


24647.964 


0.668 


190 


- 


8 


+ 


28 


14.8 


16.5 


24647.936 


0.501 


191 







+ 


24 


15.1 


16.1 


24647.981 


0.512 


192 


- 


2 


+ 


3 


15.0 


16.1 


24647.933: 


0.525 


193 


+ 


15 


- 


7 


14.8 


16.3 


24647.777 


0.630 


194 


+ 


17 


- 


13 


15.1 


16.4 


24647.758 


0.549 


195 


- 


13 


- 


29 


15.0 


16.2 


24647.470: 


0.600 



28 



Variable Stars in Globular Clusters 



No. 




x" 




y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC5272 (conti 


inued) 












196 


+ 


47 


+ 


1 












197 


+ 


58 


+ 


10 


15.1 


16.5 


24647.689 


0.500075 




198 


- 


23 


+ 


15 


15.2 


16.0 


24647.923: 


0.3617 




199 


- 


19 


+ 


13 


14.8 


16.3 


24647.699: 


0.488 




200 


- 


4 


+ 


21 












201 


+ 


4 


- 


9 


15.1 


16.1 


39964.391 


0.541333 




202 


- 


379.7 


+ 


101 


15.4 


15.8 




0.9987: 




203 


- 


30.2 


- 


308 


15.56 


15.72 




0.28719 




204 


- 


106.4 


- 


18 


15.76 


15.90 




0.9170: 




205 


- 


780 


+ 


720 


15.4 


16.2 


35600.38 


0.6369126 


vZ89 


206 







-] 


1680 


14.8 


16.1 


35601.41 


0.5093832 


vZ 1221 


207 


+ 


36.0 


- 


30.8 


14.8 


15.4 






vZ991 


208 


+ 


2.5 


- 


57.9 


14.8 


15.4 






vZ800 


209 


- 


68.2 


- 


99.1 


14.3 


15.1 






vZ472 


210 


- 


85.7 


- 


9.9 


14.6 


15.4 






vZ420 


211 


- 


54.1 


+ 


6.6 


14.6 


15.7 


41061.438 


0.557798 


vZ519 


212 


- 


21.6 


- 


38.0 


15.2 


16.2 


38867.356 


0.542196 


SVS 1365 


213 


- 


25.4 


- 


29.7 


15.0 


15.4 






vZ 648? 


214 


+ 


32.0 


+ 


5.8 


14.6 


15.6 


41061.447 


0.539493 


vZ971 


215 


- 


13.9 


- 


0.9 


14.8 


15.6 






vZ 717 


216 


+ 


27.9 


- 


10.8 


15.2 


15.8 






VZ951 


217 




0.0 


- 


26.4 


14.5 


15.4 






SVS 1370 


218 


+ 


28.1 


- 


29.4 


14.5 


15.7 


38867.304 


0.543774 


vZ950 


219 


- 


57.9 


+ 


15.7 


14.6 


15.8 






vZ509 


220 


+ 


33.1 


- 


15.2 


14.2 


14.8 






vZ978 


221 


- 


16.6 


- 


13.5 


14.6 


15.1 






vZ692 


222 


+ 


96.3 


- 


63.3 


14.9 


15.9 


38859.416 


0.596764 


vZ 1198 


223 


+ 


23.9 


- 


5.8 


14.8 


15.4 






VZ930 


224 


- 


22.1 


+ 


5.0 


13.7 


14.6 






vZ668 


225 


+ 


8.8 


+ 


225 


13.86 


14.26 


35651.38 


89.59 


vZ837 



Vars. 205. 206 found by Kurochkin, identified by Kukarkin; 207-224 by Kholopov; 225 by 
Russev. Variability of V8 and V156 reconfirmed by Kholopov, and of VI 38 by Russev. 11 sus- 
pected variables, Kholopov (1963). Identification of variables in this cluster is difficult. See von 
Zeipel numbers in S55a, with revisions by Kholopov (1963), and above for the new variables. 

Arp,AJ60.1 (1955); Roberts and Sandage, AJ 60.185 (1955); Osvath, Budapest Mitt 42 (1957); 
Kukarkin and Kukarkina, VS 12.291 (1958); Wallerstein, ApJ 127.583 (1958); Kurochkin, AC 205 
(1959); Sandage, ApJ 129.596 (1959); Kraft, Camp and Hughes, ApJ 130.90 (1959); Kukarkin, 
AC 216.29 (1960); Kurochkin, VS 13.84 (1960); Thackeray, Obs 80.226 (1960); Kurochkin, VS 
13.248 (1961); Kukarkina and Kukarkin, VS 13.309 (1961); Kurochkin, VS 14.196 (1962); Breck- 
inridge, ASP 75.22 (1963); Kholopov, VS 14.275 (1963); Fernie, ApJ 141.1411 (1965); Feast, 
ApJ 142.796 (1965); Szeidl, Budapest Mitt 58 (1965); Kheylo, IBVS 171 (1966); Sturch, ApJ 
143.774 (1966), AJ 72.321 (1967), ApJ 148.477 (1967); Kheylo, Problems in Astrophysics, Kiev, 
p. 62 (1968), NASA Tech Tr F598.57 (1971); van Albada, AAS BuU 1.366 (1969); Zhukov, Soviet 
Astr AJ 13.306 (1969); Kukarkin and Kukarkma, VS 17.157 (1970); Coutts, Bamb Veroff 9, 
100.238 (1971); Kholopov, AC 640.3 (1971), AC 651.7 (1971), AC 652.7 (1971); Russev, VS 
18.171 (1971); Kholopov, AC 676.7 (1972), Letter (1972); Szeidl, Letter (1972) 

S55a, S57, S59, S61, A62, R62a, S62, P64, S64, L65, R65, St66, S67, C&S69, 869, 870, F72 



Catalogue 



29 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC5286 a 13^43^.0, 6 -5r07' 



1 


- 46.20 


+ 145.48 


2 


+ 78.10 


- 42.63 


3 


+ 256.58 


- 39.60 


4 


- 69.30 


- 70.95 


5 


+ 64.63 


+ 27.78 


6 


+ 60.23 


- 33.00 


7 


+ 24.48 


- 60.23 


8 


+ 16.50 


- 35.75 



All above variables found by Fourcade and Laborde. One field variable, Bailey. 

Bailey, HB 801 (1924); Fourcade and Laborde, Cordoba Repr 117 (1964), Cordoba Repr 126 
(1965); Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966) 

S55a, S59, R62c, S62, F&L63, S67, S69 



NGC 


5466 a\ 


4h03ni.2,5 


+28M6' 










1 


+ 858 


- 95 


15.80 


16.80 


40706.387 


0.5774192 


+ 


2 


- 62 


-110 


15.77 


16.77 


40683.342 


0.5885020 


-,Be 


3 


- 31 


- 8 


15.90 


16.76 


40704.319 


0.5780638 


est 


4 


- 80 


+ 9 


15.69 


17.03 


40704.461 


0.5120111 


+, -,Be 


5 


- 64 


+ 112 


15.85 


17.10 


39945.659 


0.6152674 


- 


6 


+ 122 


- 24 


15.60 


16.60 


40705.408 


0.6206610 


- 


7 


-210 


-225 


15.94 


16.90 


40702.398 


0.7034205 


est 


8 


+ 23 


- 6 


15.81 


16.70 


40705.358 


0.6291182 


est 


9 


+ 31 


+ 15 


15.74 


16.77 


39947.328 


0.6850240 


- 


10 


+ 85 


+ 46 


15.87 


16.90 


40705.468 


0.7092735 


est 


11 


+ 117 


+ 68 


16.09 


16.70 


40705.285 


0.3779938 


est 


12 


+ 17 


- 88 


16.09 


16.66 


39945.210 


0.2942387 


est 


13 


- 49 


- 73 


16.10 


16.80 


40736.379 


0.3415476 


+ 


14 


- 47 


+ 52 


15.86 


16.70 


39947.568 


0.7858598 


- 


15 


+ 223 


+ 20 


16.31 


16.69 


40705.223 


0.4015471 


-, + 


16 


149 


-175 


16.04 


16.74 


39945.372 


0.2966414 


- 


17 


- 60 


- 30 


16.05 


16.58 


40706.394 


0.3701037 


+ 


18 


+ 44 


+ 41 


16.0 


16.7 


30519.697 


0.37406 




19 


+ 157 


-166 


14.40 


14.95 


40705.737 


0.8212879 


Hop 216, f 


20 


-228 


+ 45 


16.42 


16.72 






Cuffey 


21 


+ 47 


- 10 


16.53 


16.74 






Cuffey 


22 


-153 


- 80 


16.08 


16.65 


40705.364 


0.265687 


Hop 35 


23 


+ 329 


+ 15 


16.50 


16.73 


40705.126 


0.2321607 


Hop 235, est 



Baade nos. 3, 4, 5 in corona considered probable members by Kukarkin and Kholopov. Cuffey 
3-5-2-72 is considered field variable. 

Kukarkin, VS 12.50(1959); Cuffey, A J 66.71 (1961), Letters (1961); Kurochkin, VS 13.248 
(1961), VS 13.331 (1961); Kholopov, VS 14.71 (1962); Kurochkin, VS 14.196(1962); BartoUni, 
Biolchini and Mannino, Bologna Pubbl 9, 4 ( 1965); Gryzunova, AC 526.8 (1969), VS Suppl 1.253 
(1972) 

S55a, S57. S59, S61, R62a, S62, S64, L65. R65, S67, C&S69, S69 



30 Variable Stars in Globular Clusters 



No. x" y" Max. Min. Epoch Period Remark.s 



NGC5634 al4h27m.O, 6 -05°45' 



1 


-56.5 


- 19.5 


16.41 


17.39 


2 


-25.4 


+ 83.1 


16.19 


17.38 


3 


-45.1 


+ 41.9 


16.48 


17.47 


4 


+54.2 


- 65.2 


16.55 


17.39 


5 


-11.6 


-162.9 


16.72: 


17.19 


6 


+43.4 


- 52.6 


16.69 


17.05 


7 


- 0.4 


- 4.0 







0.65872 



Baade. MtWilsContr 706 (p) (1945) 
S55a, S59, S62, L65, S69 



NGC5694 al4h36m.7, 6 -26°19' 

No variables found. 
Baade, ASP 46.52 (1934) 
S55a, S59, R62c, S62, S69 



IC4499 a 14^52^.7, 6 -82°02' 

1 +84.15 - 3.03 

2 + 41.53 - 96.25 

3 - 90.75 -104.50 

4 - 33.55 - 14.03 

5 - 38.23 47.58 

6 - 2.75 + 34.38 

7 + 24.75 +203.50 

8 + 88.00 + 97.08 

9 + 72.60 +105.60 

10 + 11.00 + 68.75 

11 + 95.15 - 29.98 

12 +112.75 + 62.15 

13 + 44.28 17.33 

14 + 22.83 - 19.25 

15 - 6.88 - 9.08 

16 - 66.00 + 52.25 

17 - 22.00 + 14.58 

18 - 62.15 - 22.28 

19 -159.50 - 21.73 

20 - 22.27 +159.23 

21 + 85.53 +145.75 

22 +270.33 + 64.35 

23 + 93.50 - 38.50 

24 - 35.75 - 31.63 

25 -118.25 - 6.32 

26 -168.58 +159.50 

27 + 19.53 +111.38 

28 - 11.55 - 44.28 



Catalogue 31 

No. x" \" Max. Min. Epoch Period Remarks 

IC4499 (continued) 



29 


+ 41.25 


- 13.75 


30 


+ 85.25 


- 33.55 


31 


+ 35.75 


+ 95.70 


32 


+ 77.00 


- 11.28 


33 


+ 59.12 


-273.35 


34 


+ 88.00 


-123.75 


35 


+ 73.98 


+ 101.75 


36 


+ 159.78 


+ 6.33 


37 


+ 15.95 


- 56.10 


38 


- 85.25 


+ 56.38 


39 


+ 1.10 


+ 39.05 


40 


+ 128.98 


+280.50 


41 


+ 40.43 


+ 178.75 


42 


+ 115.50 


- 22.83 


43 


+ 64.90 


-233.75 


44 


- 62.98 


+ 61.88 


45 


+ 105.33 


+ 250.53 


46 


-133.10 


-236.50 


47 


+ 37.40 


- 93.50 


48 


+ 64.90 


- 2.75 


49 


+ 11.55 


- 99.28 


50 


+ 102.03 


- 46.75 


51 


+ 68.20 


+ 9.90 


52 


+ 63.53 


+ 178.20 


53 


+ 121.55 


-110.00 


54 


+ 93.78 


-237.33 


55 


- 46.75 


- 31.08 


56 


- 31.63 


- 9.63 


57 


- 6.05 


+ 55.00 


58 


- 58.30 


- 67.65 


59 


+ 71.23 


- 42.08 


60 


+ 2.75 


+ 54.45 


61 


+ 1.93 


+ 57.48 


62 


+ 258.23 


- 88.23 


63 


- 99.00 


- 68.20 


64 


+ 94.60 


+ 57.20 


65 


+ 30.25 


- 93.50 


66 


+ 132.00 


+ 79.48 


67 


+ 51.70 


- 13.75 


68 


- 25.03 


+ 221.10 


69 


-113.30 


+ 19.25 


70 


+ 66.28 


- 18.15 


•71 


- 30.80 


- 25.03 


72 


- 8.25 


- 69.03 


73 


+ 234.58 


-280.50 


74 


+ 22.00 


+ 66.28 


75 


+ 16.50 


- 63.25 



32 Variable Stars in Globular Clusters 



No. x" y" Max. Min. Epoch Period Remarks 

IC 4499 (continued) 



76 


+ 333.30 


+293.15 


77 


+ 79.20 


+ 52.25 


78 


-187.00 


+ 104.50 


79 


-159.50 


+316.25 


80 


+ 33.00 


-283.80 


81 


+ 45.10 


- 11.00 


82 


+ 22.55 


+ 8.25 


83 


+ 19.53 


+ 31.08 


84 


- 24.48 


- 41.53 


85 


- 91.30 


+ 309.93 


86 


+ 69.85 


+ 13.20 


87 


+ 34.93 


+ 73.98 


88 


+ 85.25 


+ 50.60 


89 


- 68.75 


- 0.83 


90 


+ 3.30 


- 19.25 


91 


- 61.05 


- 24.75 


92 


+ 123.48 


+ 138.05 


93 


+ 35.75 


- 32.18 


94 


+ 15.50 


+ 55.83 


95 


- 37.40 


+ 38.78 


96 


- 8.53 


+ 29.98 


97 


- 45.93 


- 88.28 


98 


+ 251.08 


- 44.55 


99 


-292.05 


+ 4.68 


100 


+ 72.60 


-266.20 


101 


+ 35.75 


- 20.35 


102 


+ 36.03 


+ 7.15 


103 


+ 35.48 


+ 52.25 


104 


+ 63.80 


+ 30.53 


105 


+ 72.60 


- 3.30 


106 


+ 30.25 


+ 133.93 


107 


+ 159.23 


- 81.68 


108 


+ 121.28 


+ 6.33 


109 


- 96.53 


+ 97.63 


110 


+ 38.50 


+ 82.23 


111 


+ 49.50 


-158.13 


112 


- 30.25 


+ 63.25 


113 


+ 156.75 


+ 226.88 


114 


- 7.98 


- 13.75 


115 


+ 33.28 


+ 119.08 


116 


+ 30.25 


- 31.90 


117 


-242.28 


+ 234.85 


118 


+ 168.03 


+ 181.50 


119 


- 71.50 


+ 13.50 


120 


+ 85.53 


-220.00 


121 


- 96.25 


- 31.63 


122 


+ 11.00 


- 20.63 



Catalogue 



33 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



IC 4499 (continued) 



123 


+ 164.45 


+ 17.33 


124 


+ 10.73 


+ 197.73 


125 


+ 130.35 


+ 131.18 


126 


+ 18.98 


- 59.95 


127 


+ 49.50 


- 10.45 


128 


+ 77.00 


- 38.78 


129 


- 13.20 


- 39.60 



All variables found by Fourcade and Laborde, who also have suspected variables nos. 130-169 with 
coordinates, and no. 170. 

Fourcade and Laborde, Cordoba Repr 126 (1965); Fourcade, Laborde and Albarracin, Atlas y 
Catalogo, Cordoba (1966); Fourcade and Laborde, Cordoba Repr 173 (p) (1969) 

S55b, R62b, F&L63, S67, S69, S70 



NGC 


5824 al5h00m.9, 6- 


-32"53' 










1 


- 72.8 


+ 35.5 


16.8 


18.3 


35638.20 


0.597 




2 


+ 11.3 


+ 113.1 


17.1 


18.2 


35635.48 


0.651 




3 


+ 124.7 


+ 32.0 


17.1 


18.2 


35636.42 


0.641 




4 


+ 186.5 


+ 74.0 


17.1 


18.0 






RRc? 


5 


- 9.5 


+ 108.0 


17.0 


18.1 


35638.21 


0.634 




6 


+ 98.6 


- 34.2 


17.2 


18.1 






RRc 


7 


- 36.9 


- 71.6 


17.4 


18.0 






RR 


8 


- 8.7 


- 69.4 


17.7 


18.3 






RR 


9 


+ 75.8 


+ 72.2 


16.9 


18.3 






RRa 


10 


+ 155.9 


-113.0 


17.3 


18.0 






RR 


11 


- 10.1 


- 50.8 


16.9 


17.9 








12 


- 73.3 


- 40.0 


17.0 


18.2 


35661.30 


0.592 




13 


+ 14.0 


-106.1 


17.4 


18.0 






RR 


14 


+ 19.0 


+ 51.0 


17.1 


17.9 




0.35? 


RRc 


15 


+ 82.5 


- 58.1 


17.2 


18.3 






RR 


16 


+ 4.1 


- 63.4 


17.5 


18.3 






RR 


17 


+ 33.7 


- 90.3 


17.3 


18.2 






RRc 


18 


+ 132.9 


- 3.6 


17.1 


18.2 






RR 


19 


- 29.1 


- 42.6 


17.0 


18.3 


35636.22 


0.635 


RRa 


20 


- 82.1 


- 19.8 


17.5 


18.1 








21 


+ 45.2 


+ 71.1 


17.6 


18.2 






RR 


22 


+ 48.5 


- 15.9 


17.1 


18.0 




0.6 


RRa 


23 


-125.6 


-243.2 


17.0 


18.1 


35630.23 


0.618 




24 


+ 96.3 


-305.6 


17.2 


18.0 






RRc 


25 


-333.4 


+ 6.5 


17.3 


18.1 






RR 


26 


+401.5 


+ 362.9 


17.0 


18.1 


35635.45 


0.744? 


RRa 


27 


+ 326.1 


- 24.5 


17.2 


18.1 






RR 



All variables found by Rosino. 

Rosino, ASP 73.309 (1961) 

S55b, R57, S61, S62, S64, R65. FLA66, S69 



34 



Variable Stars in Globular Clusters 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



lom 


ar5 al5 


hl3m.5, 6+0 


0°05' 








1 


- 97 


+ 25 


17.50 


17.92 


33741.651 


0.293230 


2 


- 85 


-246 


17.61 


18.01 


34456.084 


0.332467 


3 


+ 143 


-166 


17.45 


17.95 


34182.801 


0.329953 


4 


+ 35 


-238 


17.45 


17.93 


34234.522 


0.286362 


5 


- 84 


+ 94 


17.55 


17.85 


34833.520 


0.252395 



Pietra, Bologna Pubbl 6, 16 (1956); Mannino, Bologna Pubbl 6, 17 (1956); Kinman and Ro.sino, 
ASP 74.500 (1962); Rosino and Pinto, lAU Coll 21 (1973) 
S55a, R57, S59, R61, S62, S64, R65, S69 



NGC5897 a I 


5hl4ni.5, 5 


-20° 50' 










1 -109 


-201 


16.15 


17.1 


41100.695 


0.4430685 




2 - 57 


- 97 


16.25 


16.9 


36752.627 


0.454149 


var 


3 - 40 


- 4 


16.3 


17.1 


33481.615 


0.419455 


+ 


4 +71 


+ 20 


15.7 


16.2 


40807.611 


0.42 




5 -136 


+ 215 


14.85 


15.2 


40807.611 


64.5 irr 




6 +16 


+ 59 


16.4 


16.9 


41124.663 


0.3325? 


Alt 0.485 


7 +20 


+ 58 


16.2 


16.8 


40803.536 


0.511710 





Vars. 5-7 found by Sandage and Katem. Two suspected variables. 

Sandageand Katem, ApJ 153.569 (1968); Eggen, ApJ 172.639 (1972); Wehlau, Sawyer Hogg 
and Potts, JRASC 66.72 (1972), unpub (1972) 

S55a, S57,S59,S62, S69,S70 



NGC5904 (Messier 5) al5hl6m.0, 5 +02° 16' 



1 


+ 


27.7 


+ 161.1 


14.66 


15.69 


13715.588 


0.5217865 


+ 


2 


- 


343.5 


- 31.5 


14.17 


15.57 


39256.416 


0.5262679 


B2 


3 


+ 


160.1 


+ 113.7 


14.62 


15.47 


36762.676 


0.6001888 


+ 


4 


- 


12.3 


+ 73.8 


14.65 


15.89 


27627.708 


0.4496402 




5 


- 


7.8 


+ 51.6 


14.83 


16.06 


27567.929 


0.545903 




6 


+ 


27.2 


- 46.6 


14.55 


15.61 


27567.856 


0.5488311 


- 


7 


- 


5.1 


-191.3 


14.03 


15.69 


27601.730 


0.494396 


+ 


8 


+ 


134.0 


-133.2 


14.67 


15.75 


39942.309 


0.5462306 


+ 


9 


+ 


195.0 


+ 88.0 


14.57 


15.50 


27610.686 


0.6988972 


+ 


10 


+ 


107.4 


+ 382.0 


14.23 


15.45 


36762.591 


0.5306602 


- 


11 


- 


154.5 


+ 84.5 


14.27 


15.60 


36762.605 


0.5958939 


+ 


12 


- 


175.5 


- 17.3 


14.20 


15.78 


27601.762 


0.467716 


- 


13 


+ 


11.0 


- 65.4 


14.75 


15.64 


27567.800 


0.5131223 


+ 


14 


- 


145.6 


+ 103.7 


14.30 


15.62 


27610.358 


0.4871724 


-, 


15 


+ 


192.0 


+ 3.6 


14.70 


15.28 


27567.908 


0.336763 


+ 


16 


+ 


91.0 


+ 83.9 


14.29 


15.53 


27567.781 


0.6476223 


+ 


17 


- 


26.1 


+ 44.3 


14.80 


15.91 


27567.723 


0.601354 




18 


+ 


151.7 


-107.7 


14.33 


15.55 


38911.175 


0.464098 


+ 


19 


+ 


233.7 


-129.9 


14.38 


15.57 


27601.706 


0.469965 


+ 


20 


- 


255.5 


- 25.0 


14.38 


15.56 


36762.787 


0.6094778 


+ 


21 

22 


+ 


322.6 
205.7 


+ 74.0 
+ 383.5 


14.38 
not var 


15.38 


13715.505 


0.6048947 


+ 



BC 



Catalogue 



35 



No. 




x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC 5904 (continued) 












23 


_ 


253.4 


- 10.9 


not var 










24 


- 


46.8 


- 71.7 


14.77 


15.65 


27567.821 


0.4783771 




25 


_ 


28.9 


-128.0 


13.83 


14.73 


27567.766 


0.508 




26 


+ 


21.8 


+ 101.5 


14.42 


15.46 


27601.761 


0.6225642 




27 


- 


6.7 


- 59.2 


14.37 


15.74 


27888.894 


0.4703 




28 


+ 


132.2 


-121.1 


14.49 


15.59 


36762.271 


0.5439272 


- 


29 


- 


374.7 


- 76.6 


14.42 


15.53 


27567.700 


0.451433 


-, SpF 


30 


+ 


22.8 


-212.8 


14.55 


15.55 


39942.454 


0.5921739 


- 


31 


+ 


151.7 


• -141.7 


14.77 


15.48 


13715.209 


0.30058294 


est 


32 


+ 


201.9 


-150.6 


14.10 


15.67 


13715.596 


0.45778654 


est 


33 


- 


21.1 


+ 127.5 


14.57 


15.63 


27610.270 


0.5014750 


+ 


34 


+ 


84.3 


+ 59.5 


14.65 


15.52 


27567.727 


0.5681431 


est 


35 


- 


12.2 


-114.7 


14.80 


15.39 


27610.406 


0.3081255 


+ 


36 


- 


8.4 


- 52.2 


14.96 


15.91 


27563.868 


0.6277229 


est 


37 


+ 


44.7 


- 67.0 


14.49 


15.60 


27605.762 


0.4887941 




38 


- 


44.2 


+ 117.2 


14.49 


15.90 


27889.937 


0.470441 




39 


- 


125.3 


-205.2 


14.08 


15.63 


27610.368 


0.5890374 


+ 


40 


+ 


124.8 


+ 113.5 


14.84 


15.45 


27610.461 


0.3173299 


+ 


41 


+ 


19.3 


+231.4 


14.19 


15.57 


27567.879 


0.488572 


- 


42 


- 


123.2 


-120.8 


11.20 


12.24 


27567.8 


25.738 


Sp, V, mem 


43 


- 


201.8 


+ 154.3 


14.70 


15.43 


27610.364 


0.6602289 


+ 


44 


- 


102.5 


+ 31.1 


14.97 


15.61 


27610.125 


0.3296024 


+ 


45 


- 


116.7 


+ 65.7 


14.74 


15.90 


27567.774 


0.6166364 


est 


46 


- 


80.0 


+ 69.1 


not var 










47 


- 


75.3 


+ 58.1 


14.84 


15.96 


27563.861 


0.5397295 


- 


48 


- 


62.5 


+ 106.3 


not var 










49 


+ 


52.7 


+ 177.5 


not var 










50 


+ 


38.0 


+ 109.1 


14.00: 


14.54: 




irr? 


Sp 


51 


+ 


0.3 


+ 135.5 


var? 










52 


+ 


107.9 


+ 35.3 


14.49 


15.57 


27563.804 


0.5017848 


BC 


53 


+ 


68.9 


+ 19.2 


14.98 


15.28 


27601.70 


0.37360 




54 


+ 


30.3 


+ 57.2 


14.62 


15.68 








55 


+ 


80.1 


-163.2 


14.87 


15.39 


36762.219 


0.3289013 


+ 


56 


- 


68.9 


+ 96.5 


14.75 


15.86 


27889.931 


0.5346903 




57 


- 


30.6 


+ 99.7 


14.94 


15.43 


27567.897 


0.28467869 




58 


- 


605.1 


+ 168.2 


14.86 


15.52 


36762.274 


0.4912489 


+ 


59 


- 


150.0 


- 35.5 


14.70 


15.67 


13715.490 


0.5420257 


+ 


60 


- 


109.7 


+ 8.2 


15.04 


15.74 


27567.75 


0.28521 8'.' 




61 


- 


254.9 


- 31.4 


14.42 


15.62 


27610.472 


0.5686267 


+ 


62 


+ 


166.8 


-216.8 


14.78 


15.36 


36762.543 


0.2814154 


+ 


63 


+ 


212.9 


+ 51.8 


14.10 


15.50 


13384.553 


0.4976783 


+, Be 


64 


- 


51.2 


-248.9 


14.43 


15.55 


27610.553 


0.5445006 


- 


65 


- 


159.9 


- 93.8 


14.07 


15.02 


36385.522 


0.4806936 


+ 


66 


+ 


218.3 


+406.8 


14.83 


15.42 


27610.242 


0.3507086 


+ 


67 


- 


1028.2 


- 59.8 


14.36 


15.13 


13715.314 


0.3490944 


- 


68 


+ 


897.5 


+ 47.6 


14.87 


15.47 


27610.347 


0.3342667 


- 


69 


+ 


653.3 


+751.6 


14.10 


15.68 


27610.320 


0.4948729 


- 


70 


+ 


393.8 


+626.4 


14.54 


15.70 


27610.365 


0.5585490 


- 



36 



Variable Stars in Globular Clusters 



No. 




x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC 5904 (continued) 












71 


+ 


664.1 


+290.3 


14.25 


15.86 


27610.357 


0.5024724 


- 


72 


+ 


689.7 


+ 38.3 


14.66 


15.71 


27610.318 


0.5622722 


-,SpF 


73 


+ 


17.3 


+604.7 


14.66 


15.23 


19533.289 


0.3401261 


+ 


74 


+ 


202.8 


+ 162.8 


14.83 


15.18 


36762.379 


0.4539887 


- 


75 


+ 


78.6 


-412.8 


14.80 


15.38 


27610.523 


0.6854171 


+ ,SpF 


76 


+ 


80.5 


-309.2 


14.69 


15.18 


13524.125 


0.3018963 


- 


77 


_ 


171.5 


-184.8 


14.39 


15.25 


36762.596 


0.845146 


+ 


78 


+ 


65.5 


+ 159.7 


14.90 


15.46 


39942.389 


0.26481739 


est 


79 


— 


133.5 


- 32.2 


14.88 


15.42 


39942.316: 


0.33313838 


est 


80 


— 


48.6 


+ 111.6 


15.05 


15.54 


27562.986 


0.3365424 


- 


81 


_ 


72.2 


-121.7 


14.61 


15.58 


34131.439 


0.5572965 


- 


82 


_ 


67.8 


+ 12.4 


14.86 


15.72 


27563.798 


0.5584455 




83 


— 


84.7 


- 87.8 


14.80 


15.66 


27567.783 


0.5533073 


est 


84 


+ 


43.7 


- 31.9 


11.54 


12.61 


27602 


26.42 ± 


Sp, V, mem 


85 


+ 


38.3 


- 34.4 


14.80 


15.70 


27567.970 


0.52741 




86 


+ 


34.6 


- 33.0 


14.50 


15.83 


27567.856 


0.56733 




87 


+ 


122.0 


- 1.8 


15.00 


15.38 


21350.182 


0.7383992 


+ 


88 


+ 


65.2 


+ 61.8 


15.08 


15.48 


27563.832 


0.32808270 




89 


+ 


60.0 


+ 64.7 


14.79 


15.69 


27626.707 


0.55844189 




90 


— 


44.7 


+ 15.3 


14.67 


15.88 


27540.828 


0.5571527 




91 


— 


36.0 


+ 35.0 


15.04 


15.96 


27567.927 


0.584944 




92 


— 


56.6 


-123.5 


14.28 


15.58 


27567.963 


0.4635789 




93 


+ 


44.0 


- 35.7 


14.54 


15.81 


27567.771 


0.55231 




94 


_ 


23.5 


+ 17.4 


15.26 


16.11 


27601.728 


0.53141 




95 


— 


47.2 


+ 102.8 


15.13 


15.80 


27626.689 


0.29082 




96 


— 


12.4 


+ 32.9 


14.96 


16.15 


27563.778 


0.51225 




97 


+ 


48.9 


- 92.5 


14.18 


15.61 


27601.754 


0.54466 




98 


+ 


37.3 


+ 20.0 


15.26 


15.71 


27605.737 


0.3063857 


- 


99 


+ 


34.4 


- 0.1 


15.32 


15.89 


27567.739 


0.32134 




100 


+ 


2.8 


+ 48.7 


15.30 


16.01 


27628.710 


0.29434 




101 


- 


281.6 


+ 36.0 


17.15 


22 






UG? 


102 


+ 


14.8 


- 14.8 










prob RR 


103 


+ 


20.5 


- 8.8 










prob RR 



Five suspected variables, Voroshilov (1971); one suspected, Osborn (1971). 

Arp, AJ 60.1 (1955), AJ 62.129 (1957); WaUerstein, ApJ 127.583 (p) (1958). ApJ129.356 
(1959); Kraft, Camp and Hughes. ApJ 130.90 (1959); Preston, ApJ 134.651 (1961); Williams, 
AJ 71.615 (1966); Coutts, Doctoral Thesis, Toronto (1967); Sturch, ApJ 148.477 (1967); WU- 
kens, Inf Bull So Hemis 12.17 (1968); Coutts, Non-Periodic Phenomena in Variable Stars, ed. 
L. Detre, Budapest, p. 313 (1969); Coutts, Margoni and Stagni, AAS Bull 1.238 (1969); Coutts 
and Sawyer Hogg, Toronto Publ 3, 1 (1969); Kukarkin and Kukarkina, AC 541.1 (1969); Sturch, 
AJ 74.82 (1969); Zhukov, Soviet Astr AJ 13.306 (1969); Coutts Toronto Publ 3.81 (1971), 
IBVS 572 (1971); Kukarkin, AC 646 (1971); Kukarkin and Kukarkina, VS Suppl 1, 1 (1971); 
Osborn, IBVS 598 (1971); Voroshilov, AC 623.7 (1971); Coutts, Bamb Verbff 9, 100.238 (1972); 
Coutts and Sawyer Hogg, AAS Bull 4.217 (1972); Eggen, ApJ 172.639 (1972) 

S55a, R57, S57, S59, S61. A62, R62a, S62, P64, S64, L65, R65, St66, S67, S69, S70, F72 



Catalogue 



37 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC 5927 a 15h24m.4, 5 -50°29' 

L&F 4, f.' 
L&F 14 
300: Osborn 

V3, LE&M 
V6, LE&M 
V7, LE&M 
V8, LE&M 
V9, LE&M 
VIO, LE&M 
L43, LE&M 
L17,LE&M, f? 

V mags, for vars. 4-1 1, Lloyd Evans and Menzies, unpub. (1972). 13 field variables, Laborde and 
Four cade. 

Laborde and Four cade. Cordoba Repr 138 (p) (1966); Osborn, Obs 88.26 (p) (1968), Letter 
(1968): Lloyd Evans, Letter, V3 (1972); Lloyd Evans and Menzies, lAU Coll 21 (1973) 

S55b, R62b, FLA66, S69. S70 



1 


-rl41.90 


+ 129.25 






2 


- 45.38 


0.0 






3 


- 4.6 


- 4.1 






4 






14.6 


15.3 


5 






14.7 


15.2 


6 






14.7 


15.3 


7 






14.7 


15.3 


8 






15.0 


15.6 


9 







15.1 
14.7 


16.0 
15.1 


1 






14.7 


15.1 



NGC 5946 al5h3im.8,5 -50°30' 



1 


+ 178.75 


-118.25 


2 


- 56.37 


- 19.25 


3 


+ 83.87 


- 38.50 



Five field variables, Fourcade and Laborde. 

Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966) 

S55b, R62b 

NGC 5986 al5h42m.8, 6 -37°37' 



1 


+ 60.0 


- 8.3 


15.2 


16.9 


2 


- 8.0 


- 2.1 


16.1 


17.2 


3 


+ 23.2 


+ 110.5 


16.0 


17.0 


4 


-82.5 


+ 18.7 


13.6 


14.3 


5 


+ 58.6 


- 2.8 


16.1 


17.1 



All variables found by Rosino. 

Rosino, Asiago Contr 132 (p) (1962) 

S55a, R57, S59, S61, R62c, S62, F&L63, S64, FLA66, S69 



F&L 1 
F&L 2 
F&L 4 



RR? 

RR 

RR 

Slow 

RR 



NGC 


6093 (Messier 


80) a 16' 


hl4m.l, 


6-22°52' 








1 


-137 


+ 49 


13.1 


14.6 


32356.718 


16.304 


SpF-G 


. 2 


+ 22 


- 19 


13.7 


14.8 


34889.704 


24.9? 




3 


+ 104 


+ 56 


15.5 


16.15 






Short P 


4 


85 


+ 61 


15.5 


16.1 






Short P 


5 


+ 14 


- 67 


15.4 


16.3 






Short P 


6 


+ 520 


+ 296 


12.1 


16.1 


32741.67 


177.90 


S Sco, f 



38 



Variable Stars in Globular Clusters 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC6093 (continued) 
7 +502 +112 



Nova 



+ 4.0 



2.7 



11.9 
6.8 



16.3 



32770.60 
00551 



223.50 



RSco,f 
TSco 



Sawyer, Toronto Publ 1, 12 (1942); Joy, ApJ 110.105 (1949); Eggen, Royal Obs Bull 29.E73 
(1961); Kukarkin, Letter (1972); Sawyer Hogg and Wehlau, unpub (1972) 

Nova bibliography: Sawyer, Toronto Comm 1 (1938) 

S55a, S57, R57, S59, S62, R65, St66, S67, S69, S70 



NGC 6101 a 16h20m.0, 5 -72°06' 

Searched by Four cade and Laborde, but no variables found. 
Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966) 
S55b, R62b 



NGC 6121 (Messier 


•4) a I 


6h20m.6, 5 


-26°24' 








1 


_ 


281 


+ 42 


13.46 


13.97 


30000.08 


0.2888545 





2 


— 


248 


-195 


13.05 


14.10 


30000.03 


0.5356832 





3 


— 


208 


-507 


12.92 


14.08 


38500.16 


0.506651 


+ 


4 


— 


185 


^340 


11.0 


12.5 




50-70 


SpG, V 


5 


_ 


185 


- 93 


13.57 


13.99 


30000.05 


0.622398 





6 


— 


115 


+ 318 


13.54 


14.09 


30000.27 


0.320516 





7 


— 


113 


+231 


12.99 


14.28 


30000.13 


0.4987743 





8 


- 


110 


+ 111 


12.88 


14.22 


30000.18 


0.508187 


+ 


9 


- 


104 


+ 105 


12.75 


14.16 


30000.04 


0.5718975 





iO 


_ 


68 


+ 159 


12.68 


14.18 


30000.07 


0.4907173 





11 


— 


64 


-297 


13.32 


14.14 


33500.25 


0.4930721 


- 


12 


— 


53 


-207 


13.04 


14.38 


33000.40 


0.4461239 


- 


13 


- 


47 


+ 270 


12.37 


13.08 




40: 


SpG-K, V 


14 


— 


47 


-244 


12.96 


14.40 


32500.35 


0.4635338 


+ 


15 


— 


32 


+436 


12.98 


14.25 


27500.35 


0.4437857 


- 


16 


- 


29 


+ 69 


13.05 


14.18 


30000.02 


0.5425421 





17 


- 


8 


+ 20 


13.40 


13.74 








18 


+ 


4 


+ 27 


12.84 


14.20 


30000.14 


0.4787924 





19 


+ 


11 


+ 358 


12.76 


14.18 


30000.41 


0.4678111 





20 


+ 


13 


- 63 


13.24 


13.60 


30000.27 


0.309383 





21 


+ 


19 


- 4 


12.73 


14.10 


29500.11 


0.4719831 


+ 


22 


+ 


34 


+ 80 


13.40 


13.98 


31000.43 


0.6029436 


+ 


23 


+ 


38 


- 26 


13.26 


13.77 


30000.02 


0.2985502 


+ 


24 


+ 


49 


+ 48 


13.12 


14.06 


31500.53 


0.5467797 


+ 


25 


+ 


70 


+ 70 


13.08 


14.08 


30000.25 


0.6127346 




26 


+ 


94 


- 72 


12.80 


14.14 


35000.45 


0.5412163 


- 


27 


+ 


118 


+255 


12.90 


14.09 


30000.52 


0.6120191 





28 


+ 


259 


+ 84 


12.60 


14.02 


31000.05 


0.5223405 


- 


29 


+ 


326 


+598 


12.88 


14.02 


34000.19 


0.5224824 


- 


30 


+ 


340 


- 69 


13.29 


13.87 


31000.12 


0.2697490 


- 


31 


+ 


353 


+ 45 


12.72 


14.03 


31000.18 


0.5053039 


- 



Catalogue 



39 



No. 




x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC6121 (continued) 












32 


+ 


746 


- 40 


12.98 


13.96 


30000.21 


0.5791092 





33 


+ 


805 


+630 


12.70 


13.96 


30000.39 


0.6148303 





34 


— 


820 


+416 


13.16 


14.36 


29723.338 


0.554843 




35 


- 


377 


+ 62 


13.44 


14.15 


29705.441 


0.627042 




36 


— 


208 


-259 


13.26 


14.18 


29676.370 


0.541310 




37 


— 


39 


+ 2 


13.46 


13.76 


29522.064 


0.247352 




38 


— 


23 


+ 49 


13.38 


14.09 


29496.05 3 


0.577848 




39 


+ 


1 


- 80 


13.62 


14.06 


29676.463 


0.623980 




40 


+ 


25 


+ 49 








0.40151 




41 


+ 


65 


-150 


13.53 


13.97 


29676.402 


0.2517311 




42 


+ 


377 


+558 


13.33 


13.78 


29526.164 


0.303708 




43 


+ 


1263 


+ 332 


12.92 


13.48 


29748.245 


0.320637 





Joy, ApJ 110.105 (1949); Hoffmeister. Sonn Verbff 6, 1 (1963); Wilicens, La Plata Bol 7.14 (1964), 
MVS 2.101 (1964); Oosterhoff and Waliaven, BAN 18.387 (1966); Ponsen and Oosterhoff. BAN 
Suppl 1.3 (1966); Eggen, ApJ 172.639 (1972) 
S55a, S57, S59, S61, R62a, S62, S64, L65, R65, S67, C&S69. S69, S70 

NGC6139 al6h24m.3, 6 -38°44' 

Observed by Fourcade and Laborde. No variables found. 

Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966) 

S55b, R62b 



NGC6144 al6h24m.2, 5 -25°56' 

1 +481 -117 15.3 

Sawyer, JRASC 47.229 (1953) 
S55a, S57, S59,S62, S69 



16.3 



NGC6171 (Messier 


107) al 


6h29ni.7, 


6-12°57 


' 






1 


_ 


112.8 


-522.0 


14.0 


17.0 


40504. 


332 


V720 Oph, V, f 


2 


+ 


148.8 


-388.8 


15.6 


16.4 


40389.502 


0.5710205 




3 


- 


224.4 


-183.6 


15.55 


16.25 


40389.595 


0.566343 




4 


- 


99.6 


-156.6 


15.5 


16.15 


40389.628 


0.2821317 




5 


+ 


231.0 


-161.4 


15.7 


16.25 


40389.709 


0.70238 


+ 


6 


- 


10.8 


- 67.2 


15.7 


16.25 


40389.740 


0.2602558 




7 


+ 


42.0 


- 61.2 


15.6 


16.55 


40389.696 


0.499728 


+ 


8 


+ 


12.0 


- 42.0 


15.4 


16.45 


40389.957 


0.559921 


- 


9 


- 


26.4 


- 19.8 


15.95 


16.35 


40389.583 


0.3206025 


+ ? 


10 


- 


57.0 


+ 8.4 


15.4 


16.6 


40389.532 


0.4155329 


+ 


.11 


+ 


9.6 


+ 33.0 


15.8 


16.45 


40389.611 


0.592835 


_ 


12 


+ 


58.8 


+ 61.2 


15.25 


16.5 


40389.593 


0.4729722 


- 


13 


- 


27.0 


+ 72.0 


15.35 


16.6 


40389.596 


0.466797 




14 


+ 


17.4 


+ 82.2 


15.4 


16.5 


40389.763 


0.4816129 


+ 


15 


+ 


19.2 


+ 120.0 


15.6 


16.25 


40389.687 


0.2885895 





40 



Variable Stars in Globular Clusters 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC6171 (continued) 



16 


- 67.2 


+ 113.4 


15.65 


16.5 


40389.853 


0.5228709 


17 


- 99.0 


+ 71.4 


15.4 


16.45 


40389.761 


0.561154 


18 


+ 77.4 


+ 215.4 


15.75 


16.5 


40389.898 


0.564378 


19 


+ 232.8 


+ 162.6 


15.75 


16.3 


40389.822' 


0.2787622 


20 


+ 31.2 


+ 51.0 


15.65 


16.4 


40389.65 3 


0.578113 


21 


+ 81.0 


-144.6 


16.3 


16.6 


40389.704 


0.258125 


22 


-1354.2 


-183.0 










23 


- 263.4 


+ 19.2 


15.5 


16.2 


40389.725 


0.3233436 


24 


0.0 


+ 8.4 


15.65 


16.45 


40389.615 


0.3462153 


25 






14.8 






red 



prob f 



SK217, L&M 



Kukarkin, AC 216.17 (1960); van Agt, BAN 508.327 (1961); Kukarkin, VS 13.384(1961); Man- 
nino, Bologna Pubbl 7, 18 (1961); Kurochkin, VS 14.15 (1962); Kukarkin. VS 14.21 (1962); 
Coutts, Master's Thesis, Toronto (1964); Kurochkin, VS 15.164 (1964); Sandage and Katem, 
ApJ 139.1088 (1964); Sturch, ApJ 148.477, Abs. AJ 72.321 (1967); Dickens, ApJ Suppl 22.249 
(1970); Coutts and Sawyer Hogg. Toronto Publ 3.61, Abs. AAS Bull 3.242 (1971); Dickens, Letter, 
VI (1972); Lloyd Evans. Letter, V25 (1972); Lloyd Evans and Menzies. lAU Coll 21 (1973) 
S55a, S57, S59, S61, R62a, S62. S64, L65, R65, S67, S69, S70, F72 



NGC 


6205 (Messier 


13) al6h39m.9. 


6+36°33' 








1 


+ 73.06 


- 


24.86 


13.6 


15.1 


39691.720 


1.458997 


Sp A-F, V, mem 


2 


- 54.10 


- 


3.04 


12.8 


14.3 


39672.177 


5.110939 


+,Sp. V, mem 


3 


-127.70 


+ 


16.52 


15.58 


15.79 


prob not var 






4 


- 47.34 


+ 


58.18 


15.04 


15.23 


prob not var 






5 


+ 71.62 


- 


14.06 


14.33 


14.94 


40046.7820 


0.38177 




6 


+ 92.68 


+ 


76.60 


14.0 


15.1 


39664.923 


2.112867 


Sp F, V, mem 


7 


- 39.78 


- 


82.72 


14.72 


15.17 






f 


8 


- 93.02 


+ 


11.29 


14.2 


15.6 


39679.821 


0.7503158 


mem 


9 


+ 71.62 


- 


14.06 


14.0 


15.1 


40038.8121 


0.39265 




10 


- 5.40 


- 


70.7 3 


13.1 


14.0 




SR 


Sp, V, mem 


11 


- 45.78 


- 


75.88 


12.9 


13.8 




92.5 


Sp, V, mem 


12 


-105.88 


+ 


53.46 


15.0 


15.35 


prob not var 






13 


- 45.37 


- 


31.30 


14.26 


14.50 


prob not var 






14 


+ 3.18 


+: 


207.64 


16.16 


16.45 


prob not var 






15 


+ 79.03 


- 


115.34 


13.32 


13.67 




irr 


mem 


16 


+ 349.40 


+: 


207.90 










Tsoo Yu-hua 



Variable 1 6 = Savedoff A 1 8, probably Ludendorff 1113. 
One field variable, Tsoo Yu-hua. 

Joy, ApJ 110.105 (1949); Arp, AJ 60.1 (1955); Brown, ApJ 122.146 (1955); Savedoff, AJ 61. 
254(1956); Wallerstein, ApJ 127.583(1958); Kraft, Camp and Hughes, ApJ 130.90 (1959); 
Kurochkin, VS 13.248 (1961); Arp, La Plata Symp p. 87 (1962); Tsoo Yu-hua, Letter (p) (1964); 
Kadla, Pulk Mitt (Isw) 24.93 (1966); Osborn, Letter (1968), AJ 74.108 (1969), IBVS 350 (1969); 
Demers, AJ 76.445 (1971); Osborn, Letter (1972) 

S55a, S57, S59, S61, R62a, S62, P64, S64, L65, R65, S67, S69, S70 



Catalogue 



41 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC6218 (Messier 12) a 16h44m.6, 5 -01°52' 

1 +34 -62 11.9 13.2 27306.708 

Sawyer, Toronto Publ 1,2(1938); Joy, ApJ 110.105 (1949) 
S55a, S57, S59. R62a, S62, R65, S69 



15.508 



SpF-G, V 



NGC6229 al6h45m.6, 6+47°37' 



1 


- 24.6 


- 


105.5 


16.78 


17.94 


35630.542 


0.5856908 


2 


- 71.9 


■ + 


4.9 


16.95 


17.93 


35631.521 


0.5552380 


3 


-195.7 


+ 


41.3 


17.21 


17.82 






4 


- 56.8 


- 


14.3 


17.36: 


17.89 






5 


+ 14.5 


+ 


44.1 


17.25 


17.95 


35633.555 


0.5336051 


6 


+ 44.1 


+ 


41.5 


17.28: 


17.96 


27953.930 


0.559385 


7 


- 41.7 


- 


49.9 


16.84 


18.01 


27978.840 


0.506980 


8 


- 4.1 


- 


42.1 


15.47 


16.51 


35573.461 


14.845093 


9 


- 38.9 


+ 


38.3 


17.08 


17.88 


35629.516 


0.5428497 


10 


- 29.5 


+ 


72.7 


17.20 


18.00 


35629.535 


0.5547785 


11 


+ 23.9 


- 


25.0 


J17.44 


18.01 






12 


+ 34.2 


- 


23.6 


17.12 


18.02 






13 


+ 140.2 


+ 


61.3 


17.20 


17.96 


35630.552 


0.5473432 


14 


- 15.5 


- 


50.7 


16.76 


17.86 


35631.565 


0.4659161 


15 


+ 34.2 


+ 


27.5 


17.39 


17.92 


35611.460 


0.2713783 


16 


+ 47.0 


- 


24.2 


17.31 


17.94 


35637.500 


0.322784 


17 


- 96.3 


- 


75.0 


17.08 


17.72 


27979.830 


0.324880 


18 


- 36.1 


+ 


32.2 


17.34 


18.00 






19 


+ 53.4 


- 


44.4 


16.96 


18.00 


35629.546 


0.4759609 


20 


- 27.5 


- 


36.1 


16.91 


18.05 


35631.524 


0.4659728 


21 


+ 117.3 


- 


61.6 


17.12 


17.94 






22 


+ 4 


- 


7 


15.2 


16.3 







Cep 



prob slow 

For variables with periods by both Mannino and Mayer, those of Mannino are tabulated because 
they are based on more observations. 

Baade, ApJ 102.17 (p) (1945): Sawyer, JRASC 47.229 (1953); Mannino, Bologna Pubbl7, 13 
(1960); Mayer, BAG 12.167 (1961) 

S55a, 857, S59, R62a, S62, S64, L65, R65, S69 



NGC6235 a 16h50m.4, 6 -22°06' 



-16 

+ 58 



+ 39 
-211 



16.5 
16.5 



17.2 
17.3 



Sawyer, JRASC 47.229 (p) (1953) 
S55a, S57, S59, S62, S69 



NGC6254 (Messier 10) a 16h54m.5, 6 -04°02' 



+ 5 
+ 30 



+ 22 
+ 120 



13.2 
11.91 



13.8 
13.34 



34907.0 



18.728 



SpG,V 
SpF-G,V 



42 



Variable Stars in Globular Clusters 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC6254 (continued) 
3 -209 +106 



13.10 13.82 



34905.64 



7.908 



Min 

Voroshilov 
Arp IV-37 



Joy, ApJ 110.105 (1948); Arp, AJ 60.1,320 (1955), AJ 62.129 (1957); Wallerstein, ApJ 127.583 
(1958); Voroshilov, AC 623.7 (1971) 
S55a, S57, S59, R62a, S62, R65, S69 



Palomar 15 al6h57m.6, 5 


-00°28' 










No variables found. 














Kinman and Rosinc 


., ASP 74.499 (1962) 








R61 
















NGC 6266 (Messier 


62) al( 


5h58m.l,( 


5 -30°03' 








1 


+ 41.0 


+ 6.1 












2 


- 26.6 


- 68.9 










SpF-G 


3 


- 88.9 


- 6.8 






33421.41 


0.49158 




4 


- 93.9 


- 39.3 


15.68 


16.85 


33419.49 


0.54113 




5 


-163.2 


+ 123.5 


15.50 


16.53 


33417.51 


0.46049 




6 


- 81.7 


+ 34.0 






33419.30 


0.49191 




7 


+ 22.1 


+ 169.4 


15.86 


17.06 


33419.38 


0.56389 




8 


- 93.2 


+ 162.4 






33423.44 


0.53200 




9 


- 92.6 


+213.1 


15.40 


16.68 


33423.48 


0.55662 




10 


-454.0 


+ 157.7 


15.58 


16.93 


33418.45 


0.53259 




11 


-457.1 


+ 126.7 


16.06 


16.85 


33421.56 


0.59823 




12 


-204.4 


+ 268.9 






33421.39 


0.48799 




13 


+ 1.6 


+ 30.2 












14 


- 92.2 


+ 265.8 


15.27 


16.83 


33421.41 


0.44216 




15 


+ 123.0 


+ 303.4 


16.01 


16.91 


33423.60 


0.63024 




16 


- 74.5 


+ 93.9 


15.35 


16.51 


33421.55 


0.59591 




17 


- 22.1 


+ 102.4 






33423.51 


0.5251 




18 


- 33.3 


+ 92.3 


15.90 


16.80 


33423.58 


0.52616 




19 


- 14.5 


+ 65.5 






33421.53 


0.52271 




20 


+ 131.6 


+ 159.4 


15.68 


17.00 


33423.52 


0.47201 




21 


+ 105.9 


+ 79.7 


15.75 


17.14 


33421.42 


0.45045 




22 


+ 61.9 


+ 11.9 






33421.48 


0.49925 




23 


- 73.2 


- 37.4 






33417.56 


0.44821 




24 


+ 58.1 


- 38.6 






33417.59 


0.52267 




25 


+ 152.5 


- 72.8 


16.35 


17.71 


33421.45 


0.44584 




26 


-182.9 


-303.1 












27 


- 6.8 


- 59.8 






33423.40 


0.44916 


Vars. 27-42 


28 


+ 154.0 


+ 19.3 


16.81 


17.45 


33423.52 


0.49749 


discovered by 


29 


+ 153.4 


+ 14.5 


15.96 


17.35 


33423.44 


0.56 


van Agt 


30 


- 61.7 


-181.9 


16.69 


17.36 


33418.54 


0.30440 




31 


- 46.4 


-143.0 






33419.37 


0.48500 




32 


- 1.0 


-136.4 






33423.51 


0.5468 





Catalogue 



43 



No. 


x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC6266 (continued) 












33 


- 13.7 


-117.9 


16.79 


17.71 


33422.51 


0.57438 




34 


61.0 


4.9 






33422.54 


0.58372 




35 


-113.2 


+ 14.1 


15.56 


16.82 


33418.48 


0.5288 




36 


- 41.2 


+ 125.6 


15.84 


16.66 


33423.49 


0.6530 




37 


- 53.2 


+ 6.5 






33423.38 


0.5852 




38 


22.1 


- 44.8 






33421.56 


0.77083 




39 


-121.4 


+ 59.0 


16.02 


16.89 


33421.51 


0.64020 




40 


-122.0 


+ 45.6 






33423.52 


0.30131 




41 


-118.4 


+ 40.7 






33423.46 


0.55848 




42 


-130.0 


+ 50.0 


16.00 


16.35 


33421.56 


0.24765 




43 


- 62.8 


-223.1 


16.36 


17.40 


33423.37 


0.56356 


Vars. 43-82 


44 


- 47.6 


-122.7 


16.48 


17.99 


33423.54 


0.44575 


discovered by 


45 


+ 59.0 


-187.7 


16.72 


17.95 


33417.60 


0.51688 


Oosterhoff 


46 


+ 130.9 


+477.9 


16.65 


17.63 


33418.45 


0.53874 




47 


- 22.0 


+ 241.6 


16.34 


16.93 


33422.39 


0.61211 




48 


86.1 


-130.8 


16.35 


17.29 


33421.49 


0.74360 




49 


+ 139.0 


-104.7 






33423.35 


0.54360 




50 


+ 281.7 


- 34.4 


16.38 


17.65 


33421.56 


0.50264 




51 


+ 294.3 


+ 193.7 


16.40 


17.01 


33421.50 


0.26181 




52 


+ 75.9 


-181.5 


16.58 


17.87 


33423.59 


0.50538 




53 


-111.8 


-101.0 












54 


-150.5 


-671.7 






33423.51 


0.38591 




55 


+422.7 


+ 278.4 


16.07 


17.11 


33417.50 


0.47872 




56 


+ 37.1 


+ 118.9 


16.22 


17.00 


33423.47 


0.5654 




57 


+ 51.1 


+ 121.1 


16.00 


17.03 


33423.61 


0.55636 




58 


- 98.6 


+ 32.2 






33423.40 


0.48100 




59 


+ 122.1 


+ 94.1 


16.15 


17.23 


33421.46 


0.57931 




60 


+ 308.8 


+ 395.5 


15.99 


16.53 


33423.63 


0.28662 




61 


+ 215.9 


+ 190.7 


16.57 


17.25 


33421.48 


0.26602 




62 


+ 238.5 


+ 104.9 


15.99 


17.26 


33419.45 


0.54807 




63 


+ 105.4 


-102.4 


16.75 


17.55 


33418.59 


0.64313 




64 


124.6 


-266.4 


16.10 


17.08 


33422.37 


0.47299 




65 


86.6 


+ 137.5 












66 


-316.8 


+ 17.5 


16.19 


16.74 


33423.60 


0.33383 




67 


+ 399.1 


+621.4 


16.12 


17.14 


33421.44 


0.56488 




68 


+ 146.5 


+ 417.6 


16.05 


16.57 


33419.50 


0.23529 




69 


+ 122.3 


+ 109.9 


16.39 


16.94 


33423.55 


0.31369 




70 


-725.2 


- 86.9 






33423.55 


0.54546 




71 


- 87.6 


-482.4 






33422.34 


0.70452 




72 


-182.7 


-104.5 


16.09 


17.29 


33421.43 


0.46751 




73 


-203.5 


-105.5 












74 


- 21.4 


- 53.6 






33423.60 


0.46646 




75 


+ 396.5 


+ 237.5 


16.57 


17.10 


33423.43 


0.33429 




76 


+ 178.1 


+629.6 


15.81 


16.55 


33421.50 


0.61523 




77 


+ 275.3 


+ 33.1 


16.82 


17.30 








78 


+ 338.4 


+ 174.1 


16.78 


17.45 


33421.49 


0.62170 




79 


+694.3 


- 81.0 






33423.40 


0.31896 





44 Variable Stars in Globular Clusters 



No. x" y" Max. Min. Epoch Period Remarks 



NGC6266 (continued) 

80 - 85.3 + 90.4 15.90 16.74 33422.54 0.58858 

81 -110.5 + 97.3 15.65 16.95 33419.39 0.53093 

82 - 39.4 - 68.0 33421.58 0.56481 

83 - 38.3 - 9.9 van Agt 

84 16.55 17.53 G&F 

85 16.68 17.55 G&F 

86 16.38 17.69 G&F 

87 15.80 16.70 G&F 

88 16.04 16.75 G&F 

89 16.45 17.66 G&F 

Wallerstein, ApJ 127.583 (1958); van Agt and Oosterhoff, Leiden Ann 21.253 (p) (1959); Gas- 
coigne and Ford, Proc Astr Soc Aust 1.16 (1967); van Agt, Priv comm (1971); Gascoigne, Letter 
(1971) 
S55a, S57, S59, S61, R62a, S62, R65, FLA66, S69, S70 

NGC6273 (Messier 19) a 16h59m.5, 5 26° 11' 

Cap? 



1 


+ 4 


+ 48 


14.1 


15.1 


2 


+14 


+ 123 


13.4 


14.7 


3 


-28 


- 6 


14.2 


15.2 


4 


- 2 


- 24 


15.1 


15.7 



Two field variables. Sawyer. 

Sawyer, Toronto Publ 1, 14 (p) (1943) 

S55a, S57, S59, S61, R62a, S62, S69 



NGC6284 a 17hOim.5, 5 -24°41 



1 


- 24 


+ 36 


15.6 


16.1 


2 


- 47 


- 17 


16.1 


17.0 


3 


- 28 


- 13 


15.3 


15.7 


4 


+ 22 


- 18 


15.4 


16.3 


5 


+ 109 


-205 


16.4 


17.0 


6 


+ 139 


+ 221 


15.9 


16.4 



Four field variables. Sawyer. 

Sawyer, Toronto Publ 1, 14 (p) (1943) 

S55a, S59, S62, S69 



NGC6287 al7h02m.l,5 -22°38' 



1 


-152 


-40 


16.2 


17.1 


2 


+ 46 


-26 


15.7 


15.9 


3 


+ 26 


+44 


16.1 


16.8 



Three field variables, Sawyer. 
Sawyer, Toronto Publ 1, 14 (p) (1943) 
S55a, S59,S62, S69 



Catalogue 



45 



No. 



Max. Min. 



Epoch 



Period 



Remarks 



NGC6293 al7h07m.i,5 -26°30' 



1 


+ 81.0 


+49.5 


15.9 


16.6 


2 


-135.6 


+64.5 


15.8 


16.7 


3 


+ 48.6 


+ 18.6 


15.5 


15.8 


4 


+ 92 


-81 


16.1 


17.1 


5 


+ 78 


-83 


15.7 


16.5 



Three field variables. Sawyer. 

Shapley, Mt WUs Contr 190 (1920); Sawyer, Toronto Publ 1, 14 (p) (1943) 

S55a, S59,S62, S69 



NGC6304 al7hlim.4, § _29°24' 



1 


+ 102.0 


-114.4 


16.5 


18.0 


2 


-168.9 


+ 169.6 


15.7 


17.5 


3 


+ 200.5 


+ 60.2 


16.5 


17.5 


4 


-272.4 


-154.9 


16.0 


16.9 


5 


+ 235.5 


- 7.8 


16.7 


17.6 


6 


+ 304.7 


-191.7 


16.6 


17.8 


7 


+ 0.8 


-293.5 


17.5 


18.3 


8 


+ 486.7 


+ 49.9 


16.7 


17.7 


9 


+ 587.1 


+ 230.2 


16.8 


17.8 


10 


-591.2 


-247.6 


16.2 


17.9 


11 


-244.8 


-5 34.6 


16.4 


17.2 


12 






13.95 


14.30 


13 






11.00 


12.52 


14 






10.75 


13.25 


15 






12.90 


13.88 


16 






13.70 


13.80 


17 






15.25 


15.40 


18 






13.60 


[14.60 


19 






13.38 


13.78 


20 






13.91 


14.15 


21 






13.87 


14.40 



RR? 




RR 




RR 




RR 




RR 




RR 




RR 




Terzan 


28 


Terzan 29 


Terzan 


30 


Terzan 32 


Terzan 


33 


Terzan 40 


Terzan 


43 


Terzan 68 


Terzan 69 


Terzan 


72 



Vars. 1-1 1 found by Rosino, 12-21 by Terzan on red plates. Many field variables by Terzan. 

Rosino, Asiago Contr 132 (p) (1962); Terzan, Haute Prov Publ 9, 1 (1966), Haute Prov Publ 9. 
24(1968) 

S55b, R57, S61, R62c, S62, F&L63, 864, FLA66, S69, S70 



NGC6316 al7hl3m.4, 5 -28°05' 
S55b,R62b 



NGC6325 anhjsm.o, 5 -23°42' 
S55b,R62b 



46 



Variable Stars in Globular Clusters 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC 6333 (Messier 9) al7hl6m.2. 5 -18°28' 



1 


+ 91 


- 76 


15.6 


16.9 


29427.886 


0.585727 


2 


+ 40 


- 31 


15.6 


16.4 


29436.854 


0.628191 


3 


+ 207 


-210 


15.7 


16.85 


32000.735 


0.605397 


4 


+ 23 


- 35 


15.8 


16.95 


30520.749 


0.670076 


5 


+ 34 


- 7 


16.0 


16.8 


29435.870 


0.274708 


6 


- 70 


- 14 


15.7 


16.95 


29435.870 


0.607795 


7 


-111 


- 80 


15.95 


17.2 


29434.860 


0.628456 


8 


- 73 


- 99 


16.05 


16.9 






9 


+ 334 


-191 


16.0 


16.75 


30933.704 


0.322990 


10 


+ 37 


+ 26 


16.2 


16.9 


30553.653 


0.242322 


11 


- 4 


- 7 


15.7 


16.8 






12 


-275 


-136 


15.85 


16.95 


29408.951 


0.571784 


13 


+ 259 


+ 11 


16.7 


17.8 


30554.694 


0.47985 



Sawyer, Toronto Publ 1, 24 (p) (1951) 
S55a, S59, R62a, S62, L65, R65, S69 



NGC 6 341 (Messier 


92) a 17 


hl5m.6. 


6+43°12' 








1 


+ 127.5 


+ 41.3 


14.35 


15.30 


24410.198 


0.7028015 




2 


+ 91.2 


+ 69.2 


14.55 


15.25 


24409.347 


0.6438829 


BC 


3 


+ 53.7 


+252.7 


14.20 


15.35 


24410.377 


0.6375010 


-,Sp 


4 


- 76.0 


+ 58.0 


14.45 


15.20 


24433.262 


0.6289128 




5 


+ 81.6 


- 53.7 


14.50 


15.25 


24428.315 


0.6196963 


BC 


6 


+ 38.7 


+ 43.3 


14.5 3 


15.40 


27340.360 


0.600001 




7 


+ 1.6 


- 50.5 


14.45 


15.70 


37871.517 


0.5149114 




8 


+ 208.9 


+ 208.0 


14.50 


15.20 


24410.289 


0.6732769 


Sp, BC 


9 


+ 18.0 


- 48.1 


14.80 


15.60 




0.61 var 




10 


+ 83.0 


+ 36.3 


14.75 


15.20 


24410.454 


0.3773182 




11 


+ 71.2 


- 67.1 


14.80 


15.20 


24466.213 


0.3084409 


BC 


12 


- 29.9 


- 97.8 


14.70 


15.10 


38905.364 


0.409939 




13 


+ 153.4 


- 60.1 












14 


-316.0 


+ 245.7 


14.45 


14.85 


39026.410 


0.346178 


EW, f 


15 


- 2 


+ 77 


14.05 


14.55 






RR 



V15 in Second Catalogue is same as V12 (Kukarkin, Letter, 1972) so V16 renumbered 15. Nine 
field variables, Mnatsakanian and Sahakian. 

Walker, AJ 60.197 (1955); Preston, ApJ 134.651 (1961); Kheylo, IBVS 43 (1964), IBVS 104 
(1965), VoprosyAstrofiziki, Kiev, p.l24 (1966). VS 16.213(1967); Sturch, AJ 72.321, ApJ 
148.477 (1967); Bartolini, Battistini and Nasi, Bologna Pubbl 9, 15 (1968); Mnatsakanian and 
Sahakian, AC 528.5 (1969); Eggen, ApJ 172.639 (1972); Kukarkin, AC 707.7 (c) (1972) 

S55a, S57, S59, S61, R62a, S62, P64, S64, L65, R65, St66, S67, C&S69, S69, S70 



NGC6342 al7hl8m.2, 5 -19°32' 
S55b, R62b 



1 


-226.33 


-158.13 


2 


+ 130.63 


+ 58.30 


3 


-286.00 


+ 139.91 


4 







Catalogue 47 

No. \" y" Max. Min. Epoch Period Remarks 

NGC6352 al7h2im.6. 6 -48°26' 

F&L 1 
F&L 4, f? 
F&L 8 
12.7 13.4 HH113 

Fourcade and Laborde nos. 2, 3, 5, 6, 7, 9-12 considered field. V4 found by Lloyd Evans and Men- 
zies (1973), who also have one field variable. 

Fourcade and Laborde, Cordoba Repr 117 (1964), Cordoba Repr 126 (1965); Fourcade, Laborde 
and Albarracin, Atlas y Catalogo, Cordoba (1966); Hartwick and Hesser. ApJ 175.77 (1972); Lloyd 
Evans. Letter (1972); Lloyd Evans and Menzies, lAU Coll 21 (1973) 

S55b, R62b. F&L63. S67. S69 

NGC6355 al7h20m.9. 6 -26'19' 
S55b,R62b 

NGC6356 al7'i20m.7, 5 17°46' 



32328. 208: 



SW 34 

^ SW 72 

SW 30 
SVv'46 

*l-ormerly Sawyer II, which Wilkens says should be included in the cluster. Vars. 7-10 discovered 
by Lloyd Evans and Menzies (unpub). 

Sawyer. JRASC 47.229 (p)( 195 3); Sandage and Wallerstein. ApJ 131.598 (p) ( 1960); Lloyd 
Evans. Letter (1972); Sawyer Hogg, unpub ( 1972); Wilkens, Letter ( 1972); Lloyd Evans and Men- 
zies, lAUColl 21 (1973) 

S55a. S57. S59. R62c, S62. P64. R65, S69. F72 



1 


15 


- 24 


16.3 


17.2 


2 


+ 101 


-110 


16.8 


17.1 


3 


- 24 


+ 45 


16.0 


117.5 


4 


+ 187 


+ 47 


15.9 


117.5 


5 


255 


-152 


15.7 


117.5 


6* 


575 


+ 114 


15.6 


il7.3 


7 






15.4V 


15.6V 


8 






15.6V 


16.0V 


9 






15.3V 


15.7V 


10 






15.4V 


15.7V 



NGC6362 a 


\lK 


26'".6. 6 


67°or 










1 


00 




00 












2 


26 




100 












3 


83 




^ 90 












4 


79 




88 












5 


f 81 




15 












6 


+ 54 




+ 174 


14.9 


15.3 


36565.999 


0.2628878 


VH 15 


7 


+ 22 




+ 104 


13.7 


14.5 


36565.724 


0.5215674 


VH6 


8 


263 




f 108 


14.8 


15.3 


36566.080 


0.3810811 


VH 17 


9 


207 




+ 138 













48 



Variable Stars in Globular Clusters 



No. 


x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC6362 (continued) 












10 


+ 186 


+ 353 


14.5 


14.9 


36566.024 


0.3617240 


VH 10 


11 


- 29 


+ 48 












12 


-246 


-103 


14.5 


15.5 


36565.817 


0.5328711 


VH 3 


13 


-234 


-120 


14.4 


15.4 


36565.811 


0.5800254 


VH 1 


14 


+ 369 


+ 28 


15.0 


15.3 


36565.865 


0.2463744 


VH 16 


15 


+ 49 


00 












16 


+ 16 


-270 


14.2 


15.5 


36565.939 


0.5256730 


VH4 


17 


+ 201 


- 68 


14.9 


15.3 


36566.026 


0.3149808 


VHWl 


18 


+ 110 


+ 72 


14.2 


15.2 


36566.074 


0.5128892 


VH 13 


19 


+ 123 


- 25 












20 


+ 45 


- 15 












21 


+ 160 


-108 












22 


+ 182 


-313 


14.8 


15.3 


36566.058 


0.3639867 


VH 14 


23 


+ 30 


- 23 












24 


+ 71 


- 36 












25 


-356 


-212 


14.0 


15.5 


36566.150 


0.4558950 


VH 2 


26 


+ 22 


- 38 












27 


-193* 


+ 384 


14.7 


15.4 


36566.061 


0.3860821 


VH 9 


28 


+ 24 


+ 37 












29 


- 15 


- 35 












30 


- 89 


+ 74 


14.2 


15.4 


36566.162 


0.6133787 


VH5 


31 


- 33 


+ 80 












32 


+ 40 


+ 31 










L&F 


33 


+ 316 


+ 364 


14.7 


15.3 


36566.028 


0.4412499 


VH 11 



* Coordinate corrected. 

Vars. 16-31 found by van Agt (1961) seven of them independently by Van Hoof. One field variable, 

58' from centre, Shapley. 

Shapley, HB 777 (1922); van Agt, BAN 508.329 (1961); Van Hoof. Louv Publ 14, 1 31 (1961); 
Rosino and Sawyer Hogg, lAU Trans 11B.301 (1962); Fourcade, Laborde and Albarracin, Atlas y 
Catalogo, Cordoba (1966); Laborde and Fourcade, Cordoba Repr 138 (1966); van Agt, Priv comm 
(1971) 

S55a, S59, R62c, S62, F&L63, S64, L65, R65. S69 



NGC6366 a 17^25^.1, 5 -05°02' 



- 26 
+ 305 



- 42 
-390 



15.5 

15.7 



17.0 
16.8 



Sawyer, Toronto Publ 1, 5 (p) (1940) 
S55a, S59.S62, S69, S70 



Haute Provence 1 a 17^28^.5, 5 -29° 5 7' 

1 
2 
3 
4 



T248, 1964 
T249, 1964 
T361, 1965 
T362, 1965 



Catalogue 



49 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



HP 1 (continued) 

5 

6 

7 

8 

9 
10 
11 
12 
13 
14 
15 



T363, 
T364, 
T126, 
T130, 
T247, 
T251, 
T136, 
T137, 
T139, 
T142, 
T143, 



1965 
1965 
1966 
1966 
1966 
1966 
1966 
1966 
1966 
1966 
1966 



Identification of new variables only on prints, as indicated. 

Cailliatte, Lyon Pub! 5, 33 (1962). Haute Prov Publ 7. 2 (1964); Terzan, Haute Prov Publ 7, 3, 38 
(p) (1964). Haute Prov Publ 8. 1 1 (p), 12 (1965). Haute Prov Publ 8. 12 bis (p) (1966) 

R62b,S67, S69 

NGC6380 al7h3im.9. 6 39°02' 

1 -14.85 +131.45 F&L 

Four cade. Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966) 
S55b.R62b 



NGC6388 al7h32m.6. 5-44°43' 

1 
2 
3 
4 
5 
6 
7 



VI, M 

V2,M 

V3 

V4, M 

V6 

V7 

V8 

8 VIO 

9 Vll 

All variables found by Lloyd Evans and Menzies, identified on print. 

Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966); Feast, Quart JRAS 13.191 
(1972); Lloyd Evans and Menzies, lAU CoU 21 (c) (1973) 

S55b, R62b,F72 



Tonantzintla 2 a 17^3201.7, 5 -38° 32' 



1 +71.78 

2 +80.85 



+63.25 
+49.50 



F&L 

F&L 



Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966) 



50 



Variable Stars in Globular Clusters 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC6397 a 17h36m 8, 5 -53°39' 



1 


+ 210.7 


+ 448.4 


12.73 


17.53 


13727.6 


314.6 


Sp, M, V, f 


2 


-279.0 


-424.6 


14.30 


15.24 




45 or 60? 


prob f 


3 


-220.0 


- 33.5 


15.51 


16.65 


33119.320 


0.330667 


f 



Bamberg var. 866 in environs. 

Swope and Greenbaum, AJ 57.83 (1952); VVoolley, Alexander, Mather and Epps, Royal Obs Bull 
43 (1961); Feast. Obs 86.1 20 (1966); Strohmeier, Bauernfeind and Ott, Bamb Veroff 6.9 (1966); 
Swope, Letter (1969) 

S55a. S57, S59, A62, S62, P64, S64, R65, FLA66, S67, S69 



aC6401 al7h35m.6, 5 -23°53' 




1 I4.8r 


15. 2r 


2 15. 9r 


16.5r 


3 15. 2r 


15. 9r 



Terzan and Rutily have more than a hundred field variables. 

Terzan and Rutily, Astr and Ap 16.408 (p) (1972), lAU Coll 21 (1973) 

S55b. R62b 



T&R 41 
T&R 157 
T&R 164 



NGC6402 (Messier 14) a 1 


7h35m.O, 


5 03°13' 








1 


+ 17 


+ 47 


14.65 


16.1 


38191.8 


18.734 


-,SpG, V 


2 


-116 


-119 


15.8 


17.0 


38198.58 


2.794708 


SpF, V 


3 


- 3 


- 90 


16.65 


17.55 


38199.823 


0.522455 


- 


4 


+ 169 


+ 73 


17.2 


18.6 


38199.23 


0.651313 




5 


-136 


+ 90 


17.1 


18.7 


38199.61 


0.548796 




6 


+ 34 


- 77 


15.8 


16.4 








7 


+ 62 


- 97 


15.4 


16.5 


38189.56 


13.603 


+, SpF-G, V 


8 


+ 96 


+ 35 


17.8 


18.6 


38199.496 


0.686071 




9 


+ 151 


- 39 


17.0 


18.4 


38199.47 


0.538831 




10 


- 51 


-205 


17.1 


18.5 


38199.34 


0.585914 




11 


+ 196 


-223 


16.4 


18.0 


38199.59 


0.604417 




12 


+ 224 


-177 


17.1 


18.6 


38199.918 


0.503952 




13 


- 29 


-118 


17.0 


18.6 


38199.690 


0.535215 


+ 


14 


+ 54 


+ 1 


17.2 


18.1 


38199.931 


0.471857 




15 


-135 


+ 147 


16.9 


18.6 


38199.51 


0.557727 




16 


- 79 


- 36 


16.8 


18.2 


38199.40 


0.600617 




17 


-228 


+ 122 


15.5 


16.15 


38204.72 


12.085 


+, Sp. V, f? 


18 


+ 61 


- 22 


16.9 


18.15 


38199.885 


0.479065 


- 


19 


-128 


+ 2 


17.0 


18.6 


38199.34 


0.545671 




20 


-145 


+ 98 


17.9 


18.55 


38198.734 


0.263721 




21 


+ 72 


+ 125 


16.3 


17.4 








22 


+ 70 


+ 95 


17.3 


18.5 


38199.23 


0.655916 




23 


+ 74 


+281 


17.1 


18.5 


38199.72 


0.552342 




24 


- 2 


+ 75 


17.0 


18.7 


38199.64 


0.519901 




25 


- 28 


-312 


17.65 


18.4 


38199.48 


0.360707 




26 


- 85 


+ 27 


16.5 


17.5 








27 


-421 


+ 151 


16.45 


17.6 


34936 


308.0 


f? 



Catalogue 



51 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC6402 (continued) 



28 


-465 


+ 372 


15.0 


16.0 






29 


- 68 


-152 


15.7 


16.2 






30 


+ 76 


- 12 


16.9 


18.3 


38199.72 


0.534226 


31 


- 41 


+ 32 


16.8 


17.7 


38199.383 


0.619636 


32 


+ 36 


+ 147 


17.0 


18.1 


38199.55 


0.655975 


33 


-138 


+ 12 


17.3 


18.3 


38199.59 


0.479946 


34 


- 70 


+ 26 


17.8 


18.8 


38199.854 


0.606627 


35 


-112 


- 49 


16.2 


17.4 






36 


+ 204 


-346 


17.2 


18.3 


38199.33 


0.677990 


37 


+ 5 


+ 18 


17.65 


18.9 


38199.654 


0.489060 


38 


+ 11 


- 17 


16.0 


17.0 






39 


+ 46 


- 2 


16.1 


17.6 






40 


+ 253 


+ 310 


16.4 


17.1 






41 


- 13 


- 3 


16.0 


17.1 






42 


+ 36 


+ 12 


15.9 


17.1 






43 


+ 68 


+ 23 


17.0 


18.2 


38199.46 


0.521747 


44 


+ 20 


+ 116 


16.3 


17.5 






45 


- 90 


+ 94 


15.7 


16.4 






46 


+ 91 


- 66 


16.4 


17.4 






47 


89 


+ 26 


16.5 


17.6 






48 


- 4 


+ 40 


16.3 


17.7 






49 


- 98 


- 19 


16.0 


16.9 






SO 


- 15 


- 38 


16.1 


17.0 






51 


+ 104 


-305 


17.6 


18.15 


38198.709 


0.367606 


52 


+ 82 


+ 39 


16.5 


17.0 






53 


+ 134 


+ 129 


16.4 


17.3 






54 


+ 121 


+ 113 


16.6 


17.6 






55 


+ 33 


+ 106 


16.5 


17.5 






56 


- 68 


-184 


16.4 


17.4 






57 


+ 134 


-116 


16.3 


17.6 






58 


-123 


- 34 


16.4 


17.3 






59 


- 32 


+ 30 


17.4 


18.75 


38199.561 


0.555634 


60 


+ 41 


+ 54 


16.2 


17.7 






61 


+ 12 


- 43 


16.6 


17.7 


38199.610 


0.569824 


62 


-232 


-154 


18.0 


18.5 


38235.444 


0.638460 


63 


+ 122 


- 63 


16.5 


17.4 






64 


- 51 


-169 


16.5 


17.5 






65 


-125 


+ 13 


16.4 


17.2 






66 


-133 


+ 37 


16.6 


17.4 






67 


+ 34 


+ 14 


16.1 


17.5 






68 


+ 10 


- 19 


17.1 


18.7 


38199.958 


0.507217 


69 


+ 140 


+ 26 


16.6 


17.3 






70 


+ 43 


- 23 


16.0 


17.2 






71 


-116 


- 50 


17.05 


18.3 


38199.602 


0.525925 


72 


+ 122 


-119 


16.5 


17.5 






73 


+ 05 


+ 07 


16.5 


18.0 




irr? 


74 


+ 07 


+ 91 


16.5 


17.2 




irr? 


75 


+ 35 


- 12 


16.7 


18.5 


38199.737 


0.545281 



E,f? 



52 



Variable Stars in Globular Clusters 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC6402 (continued) 



76 


105 


+ 03 


16.1 


17.0 


38199.466 


77 


-110 


+ 55 


17.55 


18.10 




78 


-137 


- 5 


17.50 


18.50 




79 


- 12 


- 18 


17.40 


18.50 




80 


- 35 


-145 


17.50 


18.45 




81 


38 


-138 


17.65 


18.10 




82 


- 79 


-122 


17.65 


18.20 




83 


- 65 


- 34 


17.70 


18.50 




84 


- 44 


- 38 


17.80 


18.60 




85 


- 21 


+ 48 


17.65 


18.25 




86 


+ 64 


+ 22 


17.85 


18.75 




87 


- 74 


+ 11 


17.60 


18.60 




88 


- 78 


+ 10 


17.55 


18.55 




Nova 


+ 30 


+ 04 


16 




29071 



1.89003 



Only on plates 
of 1938 

Vars. 73-77 and Nova, Sawyer Hogg and Wehlau; 77-88, Wehlau and Potts. 

Joy, ApJ 110.105 (1949): Sawyer Hogg and Wehlau. A J 69.141 , loronto Comm 97 (p)(l964); 
Rep, Sky Tel 27.147 (p) (1964); Sawyer Hogg and Wehlau, AJ 70.678 (1965). Toronto Publ 2, 17 
(1966), Toronto Publ 2, 19 (1968); Demers and Wehlau, A J 76.916 (1971); Wehlau and Sawyer 
Hogg, unpub (1972); Wehlau and Potts, unpub (1972) 

S55a, S57, S59, S6 1, R62a, S64, R65, S67, C&S69, S69. S70 



Paiomar6 a 17^4011.6, 6 26°12' 

28 variables found in environs by Terzan, who says none is a probable chister member. 
Terzan, Haute Prov Publ 9. 1 (1966), Priv comm (1969) 
S70 



NGC6426 a 


17h42m.4,5+03"12' 










1 


-170 


+ 44 


17.30 


18.25 


35638.528 


0.61784 




2 


-204 


- 53 


17.60 


18.10 


35638.475 


0.35545 


Alt P 0.262 


3 


- 94 


33 


17.10 


17.50 


35660.484 


0.40385 




4 


- 77 


74 


17.70 


18.15 


35640.468 


0.42586 




5 


- 68 


- 22 


17.25 


1 8. 1 5 


35638.460 


0.70906 




6 


- 46 


+ 52 


17.30 


18.25 


35638.449 


0.68197 




7 


+ 10 


4 


17.4: 


18.1: 






RRa.' 


8 


- 15 


- 53 


17.4: 


18.2: 






RRa' 


9 


- 39 


85 


I 7.55 


18.05 


35638.460 


0.29009 




10 


+ 46 


+ 11 


17.55 


18.05 


35638.430 


0.36503 




11 


+ 285 


- 7 


15.40 


16.30 


35638.506 


0.46164 


V979 0ph,f 


12 


+ 33 


- 2 


17.60 


18.00 


35640.550 


0.23679 


Alt P0.191 


13 


+ 137 


215 


17.20 


18.10 


35634.437 


0.65190 





Three field variables also. 

Boyceand Hurahata. HA 109.19(1942) (HV 1 1037); Grubissich, Asiago Contr 94 (p) (1958) 

S55a, S59, S61, S62. L65, R65, S69 



Catalogue 



53 



No. 



Max. Min. 



Epoch 



Period 



Remarks 



NGC6440 al7h45m.9. 5 -20°2r 
S55b, R62b 



NGC6441 a\l^' 


*6m.8, 6 - 


1 


+ 46.20 


- 44.83 


2 


+ 36.85 


+ 23.93 


3 


+ 350.63 


- 90.75 


4 


+ 58.85 


.-176 


5 


+ 206.25 


+ 225.50 


6 


+ 30.53 


+ 48.68 


7 


- 38.50 


+485.10 


8 


-243.10 


-444.68 


9 


- 27.50 


- 47.30 


10 


+ 74.25 


60.50 



f? 

f? 



All variables found by Four cade and Laborde. 

Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966) 

S55b,R62b 

NGC6453 a 17h48m.O, 5 -34°37' 

Observed by Fourcade and Laborde. No variables found. 

Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966) 

S55b, R62b 

NGC6496 al7h55m.5,6 -44°15' 

Observed by Fourcade and Laborde. No variables found. 

Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966) 

S55b, R62b 



NGC65I7 a 17^5911.1, 6 -08°57' 
S55b, R62c 



NGC6522 a 18 


hOOm.4, 5 


30°02' 










1 


-67.5 


+ 34.4 


17.08 


17.74 


32416.672 


0.270 


G222, mem 


2 


+ 0.5 


+ 39.7 


16.79 


17.77 


32740.861 


0.47398 


G133 


3 


+ 14.7 


+ 37.2 


17.24 


17.74 


32705.874 


0.289 


G44, mem 


4 


+ 25.6 


+ 8.3 


17.27 


18.59 


32387.747 


0.563826 


G170, mem? 


5 


+66.0 


-42.6 


17.41 


18.19 


32349.871 


0.28684 


G37, mem 


6 


+96.5 


+ 30.5 


17.77 


18.23 


32416.753 


0.192392 


G247, mem? 


7 


-51.5 


+62.7 


17.02 


17.61 




irr 


G172,f 


8 


-20.2 


+ 49.6 


15.76 


17.00 


32290.987 


1.747 


G27, f 


9 


-19.5 


64.9 


16.73 


17.23 


32740.786 


0.299 


G232, f? 


10 






17.70 


mean 




0.564 


Clube 7, mem 



54 



Variable Stars in Globular Clusters 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC6522 (continued) 

G numbers those assigned by Baade and Gaposchkin. Clube's var. 7 identified on Plate 2 (1965) 
where some other numbers do not correspond with text. Membership comments from Clube 
(1972). 

Gaposchkin, VS 10.337 (p)(1955); Nassau, Spec Vat Ric 5.171 (1958); Woolley, Report of the 
Astronomer Royal (1964); Alexander, Obs 80.1 10 (1965); Clube, Royal Obs Bull 95.E383 (p) 
(1965); Terzan, Haute Prov Publ 8, 12 (p) (1965); Clube, Letter (1972); Kukarkin, Letter (1972) 

S55a, S59, S61, R62a, S62, P64, L65, R65, FLA66, S67, S69, F72 

NGC6528 al8hoim.6, 5 -30°04' 

A few variables from rich galactic field projected against this cluster, but Baade considered none of 
them a cluster member. S55a. 

Gaposchkin, VS 10.337 (1955) 

S59, S61, R62a, S62, FLA 66, S69 



NOG 6535 al8hOim.3, 5-00°18' 

1 -197 +65 16.3 

Sawyer, JRASC 47.229 (p) (1953) 
S55a, S57, S59, R62c, S62, S69 



17.3 



NGC6539 a 18h02m.l, 5 -07°35' 

One unpublished variable, Baade. S55a. 
S57,S59, R62c, S62,S69 



NGC6541 al8h04m.4, 5 43°44' 
1 -18.0 -126.0 12.5 [16 

Alcaino, Astr and Ap 13.399 (1971) 

S55a, S57, S59, R62c, S62, F&L63, FLA66, S69 



long 



Alcaino 127, 
prob mem 



NGC6544 a 18h04m.3, 5 -25°01' 
R62b 



NGC6553 al8h06m.3, 6 -25°56' 



1 


+ 186 


+ 20 


2 


+ 75 


-152 


3 


- 23 


- 38 


4 


+ 16 


- 2 


5 


- 71 


- 12 


6 






7 







0.5642 
0.5818 
0.4886 

270: 

]100 



prob f 

M 

LE&MAl 
LE&M A2 



Catalogue 



55 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC6553 (continued) 

8 
9 

10 
11 
12 
13 

14 
Nova -131: -281: 



[12 



30955 



LE&M 3 
LE&M6 
LE&M 7 
LE&M 13 
LE&M 1 4 
LE&M 24 
LE&M 33 
NSgr 1943 



Vars. 1-5 found by Thackeray, 6-14 and one suspected by Lloyd Evans and Menzies (1973). 
Shapley's two suspected variables are doubtful, Thackeray, Letter (1956). 

Lloyd Evans and Menzies, lAU Coll 21 (p) (1973). Nova: MayaU, AJ 54.191 (1949) 

S55a, R57, S59, R62a, S62, R65, St66, S69 



3C 


6558 al8h07m.O, 5- 


-31°47' 




1 


- 24.9 


- 3.2 


16.1 


17.5 


2 


- 15.6 


+ 46.6 


15.0 


15.8 


3 


+ 52.1 


+ 32.2 


16.2 


17.5 


4 


- 55.5 


- 24.2 


16.6 


17.7 


5 


- 48.1 


+ 124.7 


17.0 


17.6 


6 


- 23.3 


- 50.2 


16.8 


17.5 


7 


+ 113.5 


+ 132.4 


14.4 


15.4 


8 


- 2.2 


-183.6 


16.3 


17.4 


9 


-339.2 


- 36.6 


16.3 


17.8 



RR 


Rosino 




Rosino 


RR 


Rosino 


RR 


Rosino 


RR? 


Rosino 




Rosino 




Rosino 


RR 


Rosino 




Rosino 



Fourteen variables in field, Rosino. 

Rosino, AsiagoContr 52 (1954), AsiagoContr 132 (p) (1962) 

S55b, S57, R57, S59, S61, R62c, S62, S64, FLA66, S69 



IC1276 alshoSiT 


1.0, 6 -07^ 


'14' 










1 + 86.9 


+ 115.0 


]20.2 


22 




SR? 


SH 


2 - 15.2 


+ 23.7 


18.9 


20.0 


37468.96 


0.548 


K&R 


3 + 74.2 


- 51.4 


17.8 


22 




SR? 


K&R 


4 + 41.7 


+ 136.1 


18.8 


19.5 




SR? 


K&R 


5 -204.4 


+ 230.3 


18.8 


19.6 




SR? 


K&R 



Sawyer Hogg, JRASC 53.97 (p) (1959); Kinman and Rosino, ASP 74.501 (1962); Rosino and 
Sawyer Hogg, lAU Trans 1 IB. 301 (1962) 
S55b, S57, S62, S64, S69 



NGC6569 al8hl0m.4, 6 31°50' 



1 


- 95.1 


+ 28.9 


17.3 


18.1 


2 


- 91.9 


+ 0.3 


17.0 


18.0 


3 


+ 43.7 


+ 12.4 


16.6 


17.5 


4 


+ 116.5 


+ 202.1 


15.3 


17.3 


5 


- 20.7 


- 2.5 


17.0 


17.8 



short 
slow 



Rosino 
Rosino 
Rosino 
Rosino 
Rosino 



56 



Variable Stars in Globular Clusters 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC6569 (continued) 

Three field variables, Rosino. 

Rosino, Asiago Contr 132 (p) (1962) 

S55b, R57, S61, R62c, F&L63, S64, FLA66, S69 



NGC6584 al8hl4m.6, 6 -52°14' 
1 -82.5 -24.75 



F&L 



Nine field variables, Bailey. 

Bailey, HB 801 (1924); Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966) 

S55a, S59, R62c, S62, F&L63, S69 



NGC6624 al8h20m.5, 6 -30°23' 



+ 167.75 
+ 114.13 

- 9.63 

- 39.88 



+ 176.00 
+ 226.88 
+ 49.50 
- 20.63 



F&Ll 
F&L 2 
F&L 11 
F&L 14 



Only four of the variables in FLA 66 are listed here. The other 29 are considered field stars. 

Laborde and Fourcade, Cordoba Repr 127 (p) (1966); Fourcade, Laborde and Albarracin, Atlas 
y Catalogo, Cordoba (1966) 

S55b,R62b,S67, S69 



NGC6626(Messiei 


•28) al! 


8h2im.5, 


5 -24°54' 








1 


+ 174.0 


+ 188.5 


15.1 


16.4 








2 


- 47.3 


+ 63.1 


14.3 


14.8 








3 


- 32.9 


+ 111.0 


14.6 


15.4 








4 


- 34.5 


+ 33.6 


13.6 


14.8 


32759.765 


12.937 


SpF-G 


5 


- 44.8 


+ 16.4 


14.8 


15.6 


36040.674 


0.644360 




6 


+ 34.1 


+ 50.4 


14.3 


15.2 








7 


+ 172.2 


+ 102.7 


15.9 


17.0 








8 


+227.3 


-222.3 


15.6 


16.6 


25474.346 


0.56600 


Hoff63c 


9 


-158.6 


-252.4 


14.75 


15.7 


35696.652 


1.965 


Alt 0.6627 


10 


+ 96 


- 79 


13.5 


14.6 








11 


- 14 


+ 35 


15.0 


16.3 








12 


+ 148 


- 49 


15.0 


16.1 


35373.660 


0.578254 




13 


- 92 


- 24 


15.1 


16.7 


34893.807 


0.504027 




14 


-131 


-100 


15.6 


16.1 




0.330918 




15 


-472 


-186 


15.8 


17.0 








16 


+432 


-372 


15.9 


17.0 


36067.656 


0.5220278 




17 






12.8 


14.8 


38620 


92.8 


RV, Hoff 63a 


18 






15.4 


16.6 


28022.400 


0.5782670 


+, Hoff 63b 



Joy, ApJ 110.105 (1949); Sawyer, AJ 54.193 (1949); Hoffleit, AJ 70.307 (1965); Deery, AAVSO 
Abstr Oct. p. 3 (1968); Hoffleit, IBVS 312 (1968), IBVS 387 (1969), IBVS 660 (1972); Sawyer 
Hogg and Moorhead, unpub (1972) 
S55a, S57, S59, 862, S67, S69, S70 



Catalogue 



57 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC 6637 (Messier 69) al8h28m.l.5 32°23' 



1 


- 20 


- 9 


13.0 


15.0 


2 


-228.8 


+ 201.3 


15.9 


17.3 


3 


- 36.6 


- 78.5 


14.6 


15.8 


4 


- 17.5 


- 90.7 


14.3 


17.2 


5 


+ 8 


+ 7 


13.0 


14.5 


6 










7 













red, mem 




RR,f 




red, mem 


196 


mem 


195 


mem 




II 37, red 




III 43, red 




rVll,red 



28433 



Vars. 1 , 2, 3, 5 found by Rosino. V5 is Rosino 10, V4 is Ponson VI 894. Rosino considers his vari- 
ables 5-9 as field stars. Wilkens (Letter) suggests they may be cluster members. Identifications of 
new vars. 6-8, Lloyd Evans and Menzies (1973) from Hartwick and Sandage (1968). 

Ponson, Leiden Ann 20.431 (Star 69) (1957); Rosino, Asiago Contr 132 (p) (1962); Hartwick 
and Sandage, ApJ 153.715 (p) (1968); Catchpole, Feast and Menzies. Obs 90.63 (1970); Lloyd 
Evans and Menzies, Obs 91.35 (1971); Wilkens, Letter (1972); Lloyd Evans and Menzies, lAU 
CoU21 (1973) 

S55b, S57, R57, S61, R62c, F&L63, S64, R65, FLA66, S69, S70, F72 



NGC 6638 al8h27m.9, 6-25''32' 



Terzan 9 
Terzan 10 
Terzan 11 



Terzan's new variables identified on print. Six unpublished variables, Sawyer Hogg and Terzan 
(1972). 

Terzan, Haute Prov Publ 9, 24 (p) (1968) 

S55b,S57, R62b,S70 



NGC6642 al8h28m.4, 6 23°30' 



14.5 
14.9 



16.0 
16.0 



Hoff 145a, M 
Hoff 145b 



Two field variables, Hoffleit 137a and 137b. 
HofHeit, IBVS 660 (c) (1972) 
S55b, R62b 



NGC 6652 al8h32m.5,6 -33°02' 

Observed by Four cade and Laborde, 1966; no variables found. 
Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966) 
S55b, R62b 



58 



Variable Stars in Globular Clusters 



No. 




x" 


y" 


Ma.x. 


Min. 


Epoch 


Period 


Remarks 


NGC6656 (Messiei 


22) al 


8h33m.3, 


6 ~23°58' 








1 


- 


54.0 


- 10.0 


14.2 


15.4 


36070.678 


0.615543 




2 


+ 


158.6 


+ 69.2 


13.45 


14.25 


37113.784 


0.641717 




3 


+ 


214.7 


+420.2 


15.4 


16.6 


40063.702 


0.515485 


f 


4 


- 


4.0 


- 68.0 


13.9 


15.1 


40058.727 


0.716393 




5 


- 


178.2 


- 33.8 


12.5 


13.4 


40027.818 


92.6 


SpG,V, mem 


6 


- 


74.4 


100.0 


13.65 


14.5 


35279.755 


0.638548 




7 


- 


342.4 


+411.2 


13.65 


15.0 


35279.755 


0.649520 




8 


- 


39.5 


- 64.8 


12.0 


13.0 




irr. 


Sp G, V, mem 


9 


- 


211.2 


- 35.0 


12.8 


13.8 


32740.781 


87.71 


Sp G, V, mem 


10 


- 


39.0 


-125.0 


13.75 


14.7 


36069.643 


0.646018 




11 


- 


14.4 


+ 14.0 


13.1 


13.9 


36073.656 


1.69049 


Sp, V, mem 


12 


+ 


0.8 


- 77.8 


14.2 


14.6 


Prob. not vai 






13 


+ 


76.4 


+ 158.9 


13.9 


14.85 


35 309.730 


0.672523 




14 


+ 


250.8 


+486.4 


14.5 


17.5 


34983.6 


199.7 


Sp M, V, f 


15 


+ 


115.3 


- 83.2 


14.25 


14.75 


35279.755 


0.373248 




16 


+ 


185.0 


- 17.8 


14.25 


14.85 


35335.645 


0.325348 




17 


- 


438.0 


+ 126.0 


15.3 


16.7 


35338.7 


113.2 


f? 


18 


- 


86 


+433 


14.3 


14.7 


34927.766 


0.324960 




19 


- 


33 


+ 130 


14.3 


14.8 


35313.669 


0.384009 




20 


- 


120 


-123 


13.9 


14.6 


34927.766 


0.430060 




21 


+ 


36 


+ 88 


14.0 


14.5 


34922.732 


0.327530 




22 


- 


1089 


+213 


14.1 


15.8 


34927.766 


0.6245374 




23 


- 


5 


- 14 


13.9 


14.65 


35341.635 


0.355195 


+ 


24 


- 


26 


+ 10 


14.4 


15.5 








25 


+ 


326 


+ 375 


14.35 


14.85 


32006.740 


0.402367 


+ 


26 








15.6 


17.6 


36051.7 


309.0 


Hoff 8, 181a, f? 


27 








14.0 


15.1 


35280.720 


0.342811 


Hoff 10, 181b,f? 


28 








13.8 


14.8 


34920.7 


424.5 


Hoff 16, 173a,f? 


29 








14.5 


15.3 






Hoff 1 87b 


30 








12.8 


13.4 






Hoff 191 


31 








12.8 


13.5 






Hoff 185 


32 


- 


631 


-331 


15.4 


18.0 


34932.7 


233.35 


Watt, f ? 


33 


- 


149 


-794 


14.4 


17.0 


35308.8 


250.3 


Watt, f ? 



Sawyer, Toronto Publ 1, 15 (p) (1944); Joy,ApJ 110.105 (1949); Hoffleit, AJ 69.301 (1964), Sky 
Tel 27.274 (1964), AJ 70.307 (1965). AJ 72.71 1 (1967); Eggen, ApJ 172.639 (1972); Hoffleit, 
IBVS 660 (c) (1972); Sawyer Hogg and Wehlau, unpub (1972) 
S55a, S57, S59, R62a, S62, L65, R65, S67, S69, S70 



NGC6681 (Messier 70) a 18h40m.O, 6 -32°2r 



+ 46.1 
-104.5 



-113.0 
-581.3 



16.2 
16.1 



17.2 
17.1 



Four field variables, Rosino (1962). 
Rosino, Asiago Contr 132 (p) (1962) 
S55b, S61, R62c, F&L63, S64, FLA66, S69 



RR? 
RR? 



Rosino 1 
Rosino 3 



Catalogue 



59 



No. 


x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC 


6712 al 


I8h50m.3, 6 


-08°47' 










1 


- 63 


- 17 


16.18 


17.32 


35284.988 


0.512030 




2 


+ 69 


+ 15 


14.70 


16.00 


35007.4 


104.6 


AP Set, mem 


3 


- 28 


- 93 


16.66 


17.34 


35285.235 


0.655680 




4 


+ 179 


- 27 


16.96 


17.62 


35285.082 


0.611741 




5 


+ 67 


- 71 


16.00 


17.40 


35285.350 


0.545390 




6 


+ 18 


- 41 


16.10 


17.62 


35285.344 


0.510849 




7 


-129 


- 18 


13.10 


18.20 


35327 


190.48 


CH Set. V, mem 


8 


+ 24 


+ 60 


14.55 


16.20 


35400 


117.0 




9 


- 4 


+285 


16.80 


19: 






UG?,f 


10 


- 99 


+ 30 


15.45 


15.95 


35287 


174 




11 


-116 


-333 


16.7 


17.5 






E,f 


12 


+ 29 


+ 39 


16.00 


17.54 


35285.298 


0.502776 




13 


- 93 


+ 25 


15.98 


17.36 


35285.193 


0.562651 


Ros, San 


14 


-426 


+ 31 


15.30 


17.90 


35690.5 


202.2 


Sawyer Fl 


15 


+247 


- 38 


15.60 


16.60 




100'.' 


Har 160 


16 


-138 


+ 175 


16.8 


17.5 






Har 14LE 


17 


+ 27 


+ 49 


15.5 








Har 151 


18 


- 25 


- 1 


16.64 


17.26 


35285.123 


0.345044 


Sandage 


19 


- 13 


+ 34 


16.50 


16.92 


35285.162 


0.423900 


Sandage 


20 


+ 1 


+ 9 


16.60 


17.14 


35285.031 


0.330870 


Sandage 


21 






13.5 


13.8 






LE&M 



Sawyer, JRASC 47.229 (1953); Harwood, Priv comm (1956), Leiden Ann 21.387 (1962); Smith, 
Sandage, Lynden-Bell and Norton, AJ 68.293 (1963); Rosino, Bamb Kl Veroff 4, 40.202 (1965); 
Sandage, Smith and Norton, ApJ 144.894 (1966); Rosino, ApJ 144.903 (1966); Feast, Obs 87.35 
(1967); Lloyd Evans, Letter (1972); Lloyd Evans and Menzies, lAU Coll 21 (197 3) 
S55a, S57, S59, S61, R62a, S62, S64, R65, S67, S69, F72 



NGC 6715 (Messier 54) a 1 


8^52^.0, 


6 -30°32' 








1 


+ 


83 


+ 10 


15.8 


16.9 


35661.45 


1.34956 


Cep 


2 


- 


6 


+ 90 


16.3 


17.3 


35635.60 


0.5111 




3 


- 


14 


+ 179 


16.5 


17.6 


35630.44 


0.5010 




4 


- 


38 


+ 311 


16.6 


17.8 


35630.40 


0.4803 




5 


- 


129 


+ 45 


16.5 


17.8 


35636.34 


0.5780 




6 


+ 


194 


- 188 


16.6 


17.8 


35630.50 


0.5417 




7 


+ 


54 


- 165 


16.6 


17.5 




0.46? 


RR 


8 


+ 


365 


- 330 


15.7 


16.7 






H'.' f? 


9 


- 


67 


- 637 


16.8 


17.7 






RR 


10 


+ 


115 


- 530 


16.9 


17.6 






RR-? 


11 


- 


106 


-1086 










f 


12 


- 


220 


- 248 


15.4 


16.4 


35630.64 


0.3220 


prob f 


13. 


- 


238 


+ 451 


16.5 


17.5 






RR 


14 


+ 


240 


+ 213 


16.2 


17.4 


35630.44 


0.6892 




15 


+ 


124 


- 63 


16.6 


17.5 


35639.64 


0.5869 




16 


+ 


87 


- 917 










f 


17 


+ 


697 


- 435 


16.6 


17.6 


35665.30 


0.4660'? 





60 Variable Stars in Globular Clusters 



No. 




x" 




y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC6715 (continued) 












18 


+ 


511 


+ 


382 


16.5 


17.2 






RR? 


19 


-1260 


- 


190 










f 


20 


+ 


106 


+ 


95 


16.8 


17.2 








21 


+ 


85 


- 


231 




17.8 


var? 






22 


- 


21 


- 


167 


16.4 . 


16.7 








23 


+ 


362 


+ 


170 


16.8 


17.6 


35638.60 


0.5286 




24 


+ 


453 


+ 


55 


16.5: 




var? 






25 


- 


65 


+ 


74 


15.4 


17.2 


35628 


101± 


SR 


26 


+ 


201 


^ 


159 


16.8 


17.4 






RR? 


27 


+ 


209 


- 


306 


16.75 med 








28 


+ 


68 


+ 


161 


16.3 


17.6 


35630.45 


0.5128 




29 


- 


134 


- 


43 


16.6 


17.7 


35638.44 


0.5893 




30 


+ 


2 


+ 


80 


16.6 


17.7 






RR 


31 


- 


104 


- 


66 


16.8 


17.7 






RR 


32 


- 


181 


+ 


69 


16.5 


17.7 


35636.36 


0.5210 




33 


+ 


72 


- 


112 


16.3 


17.5 


35629.58 


0.4922 




34 


- 


61 


- 


153 


16.4 


17.6 


35636.32 


0.5053 




35 


- 


83 


+ 


54 


16.6 


17.6 


35665.36 


0.5266 




36 


+ 


129 


+ 


51 


16.5 


17.6 


35629.58 


0.5977 




37 


+ 


41 


- 


44 


17.3 


17.9 








38 


- 


69 


+ 


37 


17.1 


17.8 








39 


- 


105 


- 


63 


16.7 


17.7 






RRa 


40 


- 


56 


- 


112 


16.5 


17.5 


35630.44 


0.586 




41 


+ 


128 


+ 


45 


16.4 


17.6 


35630.45 


0.6187 




42 


+ 


70 


+ 


57 


16.8 


17.8 






RR 


43 


- 


154 


+ 


54 


16.8 


17.5 


35630.44 


0.3913 




44 


+ 


10 


- 


81 


16.6 


17.8 






RRa 


45 


+ 


117 


- 


109 


16.25 


17.6 


35630.62 


0.4889 




46 


- 


38 


- 


39 


17 


17.8? 








47 


- 


29 


+ 


96 


16.7 


17.7 


35635.60 


0.5069 




48 


+ 


254 


- 


47 


16.7 


17.6 


35635.58 


0.6849 




49 


- 


101 


- 


134 


16.8 


17.4 






RR 


50 


+ 


104 


+ 


61 


16.7 


17.5 


35630.64 


0.5635 




51 


+ 


222 


+ 


208 


16.85 


17.55 






RR? 


52 


+ 


90 


- 


50 


16.85 


17.55 






RR 


53 


- 


66 


- 


76 


16.8'.' 


17.6 






RR 


54 


- 


113 


+ 


327 


16.5 


17.6 


35629.57 


0.5713 




55 


+ 


146 


- 


205 


16.6 


17.6 


35629.58 


0.4259 




56 


- 


336 


- 


124 


16.65 


17.4 






RRc 


57 


+ 


293 


- 


31 


16.7 


17.7 




0.64? 


RRa 


58 


+ 


80 


+ 


282 


16.5 


17.5 


35630.50 


0.6148 




59 


- 


218 


- 


254 


16.8 


17.75 


35630.63 


0.5993 




60 


- 


269 


- 


247 


16.8 


17.6 


35629.57 


0.570? 


RR 


61 


- 


43 


+ 


107 


17.05 


17.85 






RR 


62 


- 


92 


+ 


102 


17.0 


17.8 






RRc? 


63 


- 


40 


- 


133 


16.9 


17.6 






RR 


64 


+ 


259 


- 


498 


16.7 


17.5 






SR 



Catalogue 



61 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC6715 (continued) 



65 


+ 


243 


+ 


165 


16.25 


17.05 


35638.36 


66 


+ 


234 


+ 


207 


15.6 


17.1 




67 







+ 


69 


16.85 


17.55 




68 


- 


643 


+ 


337 


16.8 


17.7 


35630.65 


69 


- 


328 


+ 


283 


16.45 


17.25 




70 


+ 


128 


- 


426 


16.8 


17.4 




71 


- 


32 


+ 


106 


14.8 


16.2 




72 


- 


61 


+ 


149 


15.6 


16.7 




73 


+ 


26 


+ 


62 


17.0 


17.5 




74 


+ 


113 


- 


141 


16.7 


17.5 




75 


+ 


18 


+ 


79 


16.5 


17.7 


35638.36 


76 


- 


106 


- 


22 


16.5? 


17.5? 




77 


- 


112 


- 


42 


16.5 


17.5 




78 


+ 


73 


- 


13 








79 


+ 


30 


- 


46 


16.9 


17.5 




80 


+ 


51 


- 


25 


16.7? 


17.5 




81 


+ 


45 


+ 


12 








82 


- 


49 


- 


46 


16.7? 


17.5? 





Vars. 29-82 found by Rosino and Nobili. 

Rosino and Nobili, Asiago Contr 97 (p) (1959) 

S55a, R57, S57, S59, S61, R62a, S62, L65, R65, FLA66, S69 



0.4481 



0.5414 



77: 



0.5797 



f 

SR 

RR 

RR*? 

RR 

SR 

E? 

RR 

RR 
RR 

RR? 



NGC6717 al8h52m.i,6 -22°47' 
S55b,S61 



NGC6723 al8h56>Ti.2, 5 -36°42' 



1 


+ 75.1 


-199.5 


15.76 


16.25 


38993.793 


0.538177 


2 


+ 135.7 


- 78.3 


14.71 


16.47 


38993.951 


0.5035 39 


3 


-244.4 


+ 7.5 


14.78 


16.57 


38994.131 


0.494097 


4 


+ 16.8 


+ 77.4 


14.55 


15.90 


38993.855 


0.451060 


5 


- 4.7 


+ 51.0 


15.20 


16.00 




0.57264 


6 


+ 7.2 


+ 48.3 


14.90 


16.05 


23618.80 


0.4814 


7 


+ 197.5 


- 71.3 


15.53 


16.14 


38994.037 


0.307672 


8 


+ 15.9 


+ 10.8 


14.75 


15.60 




0.53 


9 


+ 74.0 


+ 15.7 


14.70 


15.80 


38994.101 


0.575803 


10 


+ 148.6 


+ 83.9 


15.39 


16.03 


38993.996 


0.252325 


11 


+ 133.3 


+ 228.8 


14.85 


15.65 


38993.922 


0.534283 


12 


+ 43.2 


- 45.7 


14.95 


15.85 


23618.53 


0.4694 


13 


- 46.2 


- 71.3 


14.69 


16.22 


38993.930 


0.507867 


14 


+ 38.2 


- 43.2 


14.95 


15.80 


23618.91 


0.6190 


15. 


- 93.4 


+ 167.5 


14.72 


16.43 


38993.847 


0.435439 


16 


- 46.5 


+ 93.3 


14.55 


15.69 


38994.104 


0.696273 


17 


+ 43.1 


-102.5 


15.27 


16.66 


38994.135 


0.530179 


18 


137.8 


- 18.2 


15.40 


16.27 


38994.091 


0.526455 


19 


169.4 


-112.5 


15.24 


16.63 


38994.018 


0.534111 



62 



Variable Stars in Globular Clusters 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC6723 (continued) 



20 


+ 3.5 


+ 39.9 








0.49293 


21 


- 79.0 


- 28.2 


14.50 


15.72 


38993.760 


0.594863 


22 


- 70.8 


+ 38.1 


15.18 


15.72 


38994.19 


0.30844 


23 


+ 53.4 


- 10.0 






38994.08 


0.6259 


24 


+ 117.5 


-112.0 


15.50 


16.11 


38993.999 


0.300143 


25 


+ 98.6 


+ 203.1 


12.1V 


13.0V 




SR? 


26 


-197.0 


+ 155.9 


12.2V 


13.1V 




SR? 


27 


-219.1 


+ 101.6 


15.50 


16.33 


38994.093 


0.619249 


28 


+ 10.8 


- 79.0 








0.4863 


29 


+ 12.4 


+ 63.6 








0.53: 



F&L 



New coordinates for all variables, Menzies (1973), who discovered vars. 21-29. 

Innes, UOC 37.300 (UY Cr A) (1917); Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cor- 
doba (1966); Menzies, Proc Astr Soc Aust 1.16 (1967), Doctoral Thesis, Australian Nat'l Univ 
(1967); Lloyd Evans, Letter (1972); Lloyd Evans and Menzies, lAU Coll 21 (1973); Menzies, lAU 
CoU21 (1973) 

S55a, S59, S62, L65, R65, S69 



NGC6752 a 19h06m.4. 5 -60°04' 



+ 236.5 
+ 44.0 



+ 143.0 
+ 82.5 



F&L 
F&L 



VI considered the same as that mentioned in S55a. 

Fourcade, Laborde and Albarracin, Atlas y Catalogo, Cordoba (1966); Eggen, ApJ 172.639 
(1972) 

S55a, S57, S59, R62c, S62, F&L63, S69 



NGC6760 a 19h08m.6, 5 +00°57' 



1 


+57 


- 57 


15.7 


17.0 


2 


- 6 


-100 


16.7 


17.2 


3 


+ 31 


- 10 


15.5 


[17.4 


4 


+42 


+ 39 


15.4 


(17.5 



Taffara has new eclipsing variable in field, and gives periods for it and two other field eclipsers. 
Sawyer Hogg, lAU Agenda and Draft Reports, p. 560 (1967); Taffara, SAl 43.481 (1972) 
S55a, S57, S59, R62a, S62, S69 



NGC6779 (Messier 


56) al9hl4m.6, 


6+30°05' 








1 + 44.69 


+ 74.10 


15.0 


16.2 


30899.341 


1.510019 


Cep, Sp, V, mem 


2 + 18.16 


+ 33.09 


15.1 


15.6 




SR 




3 + 25.10 


+ 91.69 


14.4 


15.1 




SR 


Sp, V, mem 


4 -112.13 


-159.46 


15.9 


16.4 








5 + 6.79 


-134.78 


14.4 


15.2 




SR 




6 - 2.02 


+ 37.06 


12.9 


14.8 


30172.7 


90.02 


RV, Sp, V, mem 


7 +293.48 


-213.24 


15.6 


16.3 




irr 





Catalogue 



63 



No. x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC6779 (continued) 












8 - 97.63 


-335.90 


15.9 


16.7 




SR 




9 +177 


+525 


15.6 


16.1 




SR 




10 -431.53 


+ 88.33 


16.4 


17.4 


30967.473 


0.5988948 


RR,f? 


11 -415.58 


+ 283.80 


15.5 


16.3 


34239.516 


0.0756252 


RRs.f? 


12 -243.96 


- 95.41 


15.6 


16.4 









Field variables found by Kurochkin, 20 (1968), 21 (1970), 30 (1971). 

Joy, ApJ 110.105 (1949); Sawyer, JRASC 43.38 (1949); Balazs, Budapest Mitt 30(1952); 
Rosino, Asiago Contr 1 17 (1961); Preston, Krzeminski and Smak, ApJ 137.401 (p) (1963); Bar- 
bon, Asiago Contr 175 (p)(1965); Kurochkin, VS 16.460(c) (1968), VS 17.186 (c) (1970), VS 
17.620(c) (1971) 

S55a, S57, S59, R62a, S62, S64, R65, S67, S69, S70 



Palomar 10 a 19hl6m.O, 5 +18°28' 

VI found by Rosino (1972) on red plates, centre of cluster, large amphtude. 

Rosino, Letter (1972) 

R61,S61 



NGC6809 (Messier 55) a 19^36^.9, 5 -31°03' 



1 


+ 304.2 


- 55.6 


2 


-214.9 


- 26.0 


3 


+ 78 


-304 


4 


+ 108 


+ 59 


5 


41 


- 74 


6 


+ 111 


- 20 



32413.39 
32467.18 
32413.22 
32413.34 



32413.32 



0.57997286 

0.4061601 

0.6619023 

0.3841702 

0.2? 

0.388904 



Bailey, HA 38.243 (p) (1902); King, HB 920 (1951) 
S55a, S57, S59, S61, R62a, S62. R65, FLA66, S69 



Palomar 1 1 a 19^2^.6, 6 -08° 09' 

No variables found. Abell suggests this may be very rich open cluster. 

Kinman and Rosino, ASP 74.499 (1962) 

R61,S61 



NGC6838 (Messier 71) al9h5im.5, 5+18°39' 



1 


+ 140 


+ 24 


13.5 


14.9 




2 


+ 44 


-146 


13.8 


14.7 




3 


+ 44 


- 70 


15.2 


17.0 


33481.78 


4 


+ 266 


+ 31 


14.7 


15.3 





193 



3.7907 



Z Sge, SR 

Slow 

E, Min, mem 

RR? 



Silbernagel, AN 192.450(1912); Sawyer, JRASC 47.229 (1953); Prochazka, Letter (1967); Hart- 
wick, Priv comm (1972); Kukarkin, Letter (1972); Sawyer, unpub (1972) 
S55a, S57, S59, S61, R62a, S62, P64, R65, St66, S69 



64 



Variable Stars in Globular Clusters 



No. 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC 6864 (Messier 75) a 20h03m.2, 5 -22°04' 



1 


+ 15.6 


-83.4 


2 


- 9.0 


+ 54.0 


3 


+ 18.0 


+ 85.5 


4 


- 18.0 


-84.6 


5 


+ 108.0 


-36.0 


6 


+ 8.4 


81.0 


7 


- 24.6 


+ 78 


8 


- 13.5 


41.4 


9 


+ 45.6 


-24.0 


10 


- 43.5 


+ 50.4 


11 


+ 121.2 


+ 84.0 


12 


+ 39.6 


+ 75.0 



* Suspected. Four additional suspected variables, numbered 1 3-16, are omitted. 
Shapley, Mt Wils Contr 190 (p) (1920) 
S55a, S57, R57, S59, S61, S62, S64, S69, S70 



NGC 6934 a20h3 


im.7, 5+07°14' 










1 


- 45 


- 39 


16.5 


17.7 


27307.968 


0.568099 




2 


- 40 


- 14 


16.4 


17.9 


27658.930 


0.48195 


+ 


3 





+ 58 


16.6 


17.8 


27275.882 


0.539806 




4 


+ 39 


+ 58 


16.3 


17.8 


27275.882 


0.616422 




5 


+ 59 


+ 221 


16.7 


17.8 


26923.943 


0.564560 




6 


- 27 


- 33 


16.7 


18.0 


27275.941 


0.5558418 




7 


+ 92 


+ 59 


16.65 


17.7 


28038.833 


0.644049 




8 


+ 100 


+ 50 


16.75 


17.5 


27715.760 


0.623989 




9 


+ 63 


+ 18 


16.5 


17.8 


27308.844 


0.549156 




10 


-135 


+ 72 


16.4 


17.8 


27275.882 


0.519959 


- 


11 


+ 17 


+ 28 


17.1 


18.15 








12 


+ 29 


- 44 


16.3 


17.4 


27309.955 


0.464215 




13 


- 47 


+ 25 


16.55 


17.8 


26915.956 


0.551334 




14 


- 7 


- 90 


16.5 


17.8 


27659.902 


0.52199 




15 


+ 10 


- 53 


15.65 


16.3 






not RR 


16 


+ 36 


+ 18 


16.7 


17.9 


26915.956 


0.60485 3 




17 


- 73 


-107 


16.7 


17.9 


27309.955 


0.598272 




18 


+ 49 


- 8 


16.6 


17.7 






RR 


19 


+ 30 


+ 1 


16.4 


17.9 


21515.710 


0.480550 




20 


- 26 


+ 17 


16.5 


17.6 


27307.886 


0.548225 




21 


- 35 


- 3 


16.6 


18.15 






RR 


22 


-240 


-173 


16.5 


17.8 






RR 


23 


- 31 


- 16 


16.85 


18.05 






RR 


24 


+ 37 


- 53 


16.8 


17.95 






RR 


25 


+ 50 


+ 37 


16.5 


17.9 


27275.795 


0.509086 


- 


26 


+ 31 


-196 


16.9 


17.8 






RR 


27 


-148 


+ 180 


16.7 


17.8 


27272.914 


0.592204 




28 


-234 


+ 100 


16.3 


17.8 


27715.760 


0.485151 


+ 



Catalogue 



65 



No. 




x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC6934 (continued) 












29 


- 


85 


183 


16.4 


17.8 


26628.689 


0.454818 




30 


+ 


161 


+ 127 


16.6 


17.65 


27714.745 


0.589853 




31 


+ 


146 


-101 


16.5 


17.8 


21481.825 


0.505070 




32 


- 


10 


+ 51 


16.4 


17.7 


21481.825 


0.511948 




33 


+ 


37 


+ 12 


16.5 


17.7 


27309.920 


0.518445 




34 


- 


21 


+ 16 


16.6 


18.05 






RR 


35 


+ 157 


-142 


16.6 


17.85 


27664.870 


0.544222 




36 


+ 


10 


- 35 


16.05 


17.55 






RR 


37 


+ 


23 


+ 10 


16.5 


17.95 






RR 


38 


+ 


12 


- 18 


16.6 


18.0 


21543.702 


0.523562 




39 


+ 


8 


- 16 


16.6 


17.95 








40 


- 


8 


+ 26 


16.15 


16.8 






RR 


41 


+ 


30 


- 39 


16.6 


17.9 


27275.882 


0.520404 




42 


+ 


55 


+ 20 


16.5 


17.9 


27659.975 


0.524251 




43 


+ 


21 


+ 27 


16.4 


17.4 








44 


- 


43 


- 30 


17.0 


17.9 


26925.933 


0.630384 




45 


- 


32 


- 9 


16.3 


17.8 








46 


+ 


14 


- 24 


16.9 


18.05 








47 


+ 


10 


- 26 


16.8 


17.95 






RR 


48 


+ 


33 


+ 52 


16.5 


18.05 






RR 


49 


+ 


13 


- 55 


16.7 


17.95 






RR 


50 


+ 


15 


- 37 


16.9 


17.95 








51 


+ 


7 


- 25 


15.85 


16.6 






RR 



Sawyer, Toronto Publ 7, 5 (p) (1938); Sawyer Hogg and Wehlau, 
in press (1973) 
S55a, S57, S59, S61, S62, S64, R65, S67, S69, S70 



unpub (1972); Harris, AJ 78, 



NGC 


6981 (Messiei 


■72) a20h50m.7. 


6-12°44' 






1 


+ 


43.5 


- 


54.0 


16.45 


17.25 


33129.400 


0.619818 


2 


+ 


99.0 


+ 


194.4 


16.29 


17.95 


33126.405 


0.46526213 


3 


- 


52.5 


- 


58.5 


16.16 


17.74 


33809.553 


0.4976052 


4 


- 


106.5 


+ 


37.5 


16.56 


17.74 


33147.462 


0.5524863 


5 


- 


38.4 


- 


21.6 


16.40 


17.43 


22163.738 


0.4991 


6 


+ 


78.0 


+ 


78.6 


16.70 


17.10 






7 


- 


3.6 


+ 


55.5 


16.36 


17.53 


39318.997 


0.524630 


8 


- 


6.6 


+ 


89.4 


16.73 


17.74 


33145.372 


0.5683752 


9 


+ 


11.4 


+ 


50.4 


16.73 


17.54 


39319.660 


0.60296 


10 


- 


48.6 


- 


73.5 


16.69 


17.77 


33857.504 


0.5581814 


11 


+ 


57.0 


- 


36.6 


16.81 


17.72 


39319.478 


0.51997 


12 


+ 


9.0 


- 


21.6 


16.31 


17.17 


22163.90 


0.4111 


13 


+ 


13.5 


+ 


17.4 


15.77 


16.85 


39319.330 


0.55114 


14 


- 


13.5 


+ 


36.0 


16.40 


17.06 


22163.90 


0.5904 


15 


- 


64.5 


- 


21.0 


16.63 


17.56 


39318.917 


0.55044 


16 


- 


4.5 


- 


19.5 


16.31 


17.21 


39319.490 


0.585497 


17 


+ 


3.6 


- 


43.5 


16.57 


17.62 


33215.483 


0.5735404 


18 


- 


26.4 


- 


37.5 


15.70 


16.28 


22162.88 


0.52016 



66 



Variable Stars in Globular Clusters 



No. 



Max. Min. 



Epoch 



Period 



Remarks 



NGC6981 (continued) 



19 


+ 3.0 


+ 112.5 


17.15 


17.30 


not var 




20 


- 54.6 


+ 15.0 


16.50 


17.40 


33857.420 


0.595046 


21 


- 82.5 


+ 12.6 


16.56 


17.86 


33145.370 


0.5311636 


22 


-113.4 


+ 1.5 


17.10 


17.25 


not var 




23 


- 99.0 


+ 116.4 


16.95 


17.73 


39319.437 


0.585083 


24 


15.6 


- 24.0 


16.20 


16.55 


22161.92 


0.4973: 


25 


-133.5 


+ 67.5 


16.92 


17.48 


33481.810 


0.3533739 


26 


- 91.5 


- 45.0 


16.90 


17.20 






27 


+ 209.4 


-234.0 


16.30 


17.78 


39319.557 


0.673774 


28 


+ 65.4 


+ 81.0 


16.83 


17.64 


33853.437 


0.56724873 


29 


+ 36.0 


- 52.5 


16.68 


17.48 


39319.295 


0.605497 


30 


+ 71.4 


- 97.5 


16.50 


16.90 






31 


+ 5.4 


+ 36.6 


16.44 


17.36 


39319.110 


0.53249 


32 


-138.0 


- 42.0 


16.84 


17.78 


39319.440 


0.52834 


33 


+ 2.4 


- 60.6 


16.95 


17.25 






34 


- 6.0 


+ 7.5 


16.06 


16.73 






35 


+ 231 


+ 27 


16.78 


17.75 


39319.772 


0.543771 


36 


- 12 





16.0 


16.8 






37 


+ 7 


- 8 


15.5 


16.5 






38 


+ 5 


- 9 


16.6 


17.3 






39 


+ 195 


+ 243 


16.8 


17.6 






40 


+ 18 


+ 16 


16.4 


17.4 






41 


- 15 


- 20 


16.7 


17.5 






42 


+ 12 


+ 3 











f? 



red 

Nobili, Asiago Contr 83 (1957); Dickens and Flinn, MN 158.99 (1972); Dickens, Preprint (p) 
(1972), Letter, V42 unpub (1972) 
S55a, S57. S59, R62a, S62, S64, L65, R65, S67, S69 



NGC7006 a20h59m.i, 5 +16°00' 



1 


-177.9 


+ 


114.8 


18.20 


19.60 


26918.939 


0.492729 


2 


- 35.3 


- 


37.3 


18.25 


19.50 


35453.245 


0.586986 


3 


- 24.4 


+ 


34.2 


18.55 


19.65 


27209.945 


0.560557 


4 


- 21.0 


- 


41.1 


not var 








5 


- 20.9 


+ 


38.4 


18.45 


19.50 


35419.240 


0.534713 


6 


- 13.5 


- 


44.5 


18.40 


19.60 


27039.626 


0.498030 


7 


+ 3.2 


- 


36.9 


not var 








8 


+ 34.4 


+ 


13.5 


18.70: 


19.50 


35342.700 


0.608289 


9 


+ 39.4 


+ 


16.6 


not var 








10 


+ 42.8 


- 


11.8 


18.45 


19.80 


35403.638 


0.542907 


11 


+ 148 


+ 


50 


18.35 


19.65 


35428.232 


0.576036 


12 


+ 122.0 


- 


64.0 


18.35 


19.55 


35419.410 


0.574039 


13 


+ 102.7 


+ 


40.2 


18.30 


19.60 


35453.274 


0.551647 


14 


+ 35.3 


+ 128.3 


18.35 


19.55 


35459.269 


0.560358 


15 


- 11.5 


+ 114.8 


18.40 


19.50 


35429.250 


0.588067 


16 


- 39.6 


+ 


135.5 


18.35 


19.55 


35429.240 


0.537582 



Catalogue 



67 



No. 




x" 




\'" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC 7006 (continued) 












17 


- 


99.3 


+ 


85.5 


18.35 


19.60 


35429.201 


0.511494 




18 


- 


29.6 


- 


89.5 


18.55 


19.65 


35034.330 


0.603706 




19 


- 


0.6 


- 


25.3 


16.70 


17.90 


35630.93 


92.17 


red SR 


20 


- 


21.2 


- 


24.4 


18.70 


19.45 


35003.270 


0.577476 




21 


- 


21.5 


- 


18.4 


18.60 


19.50 


34978.700 


0.568968 


2 Alt Ps 


22 


- 


12.6 


- 


15.8 


18.40 


19.60 


35727.400 


0.526927 




23 


- 


27.6 


- 


7.5 


18.50 


19.60 


27274.873 


0.608042 




24 


~ 


25.8 


- 


2.9 










blended 


25 


- 


19.2 


+ 


5.2 


18.80 


19.60 


26975.580 


0.532792 




26 


- 


10.6 


- 


2.9 


18.55 


19.60 


34978.710 


0.607364 


Alt 0.540 


27 


- 


11.8 


+ 


0.3 


18.30 


19.25 


26975.650 


0.522321 




28 


- 


15.8 


+ 


4.3 


18.75 


19.60 


35657.925 


0.560987 


Alt 0.5619 


29 


+ 


35.0 


+ 


31.6 


18.40 


19.60 


27033.640 


0.559195 




30 


+ 


5.2 


+ 


16.6 


18.70 


19.70 








31 


+ 


10.0 


+ 


11.2 


18.65 


19.55 


26891.945 


0.563126 




32 


+ 


20.9 


+ 


13.8 


18.50 


19.50 


36376.920 


0.585572 




33 


+ 


31.9 


+ 


22.4 


18.50 


19.50 


34978.735 


0.556812 




34 


+ 


26.4 


+ 


9.2 


18.75 


19.30 


prob not var 






35 


+ 


36.2 


- 


2.0 


18.60 


19.55 


35419.260 


0.596309 


Pvar? 


36 


+ 


25.5 


- 


3.7 


18.75: 


19.35 


27274.850 


0.437847 


2 Alt Ps 


37 


+ 


18.9 


- 


3.4 


18.40: 


19.45 


37274.860 


0.567920 


blended 


38 


+ 


21.5 


- 


18.4 


18.70 


19.50 


26919.700 


0.608599 


Alt 0.622 


39 


+ 


11.5 


- 


25.3 


18.50: 


19.55 


36426.865 


0.577261 


Alt 0.565 


40 


+ 


9.7 


- 


14.3 


19.15: 


19.60: 






not RR 


41 


+ 


1.4 


- 


11.2 


18.70 


19.60 


34978.725 


0.495330 


Alt 0.499 


42 


+ 


9.5 


- 


7.5 


18.80: 


19.30: 








43 


- 


4.0 


- 


28.7 


18.75 


19.50 


26975.650 


0.596656 




44 


+ 


133.9 


-: 


174.0 


18.55 


19.41 


35017.632 


0.58779 




45 


- 


190.0 


- 


74.4 


18.70 


19.38 


35419.398 


0.583858 




46 


-. 


125.6 


- 


54.7 


18.85 


19.31 


35719.429 


0.666320 


Alt P? 


47 


-: 


183.4 


- 


22.1 


18.60 


19.35 


35428.253 


0.568294 




48 


-: 


100.0 


+ 


90.3 


18.70 


19.28 


35428.240 


0.611975 




49 


+ 


4.8 


+ 


40.5 


18.65 


19.60 


26891.947 


0.581897 




50 


- 


42.9 


- 


7.6 


18.60 


19.45 


35034.300 


0.590428 




51 


+ 


54.3 


+ 


46.0 


18.90 


19.35 


26918.700 


0.642709 




52 


- 


1.0 


+ 


85.5 


18.60 


19.34 


35419.290 


0.621746 




53 


+ 


47.5 


- 


9.1 


18.75 


19.25 








54 


+ 


3.2 


- 


30.0 


16.95 


17.75 






red SR 


55 


-: 


254.4 


+ ; 


504.4 


18.40 


19.60 


35017.663 


0.537740 




56 


- 


10.7 


- 


11.8 


18.75 


19.55 


36376.920 


0.520202 


Alt 0.549 


57 


- 


6.2 


- 


12.1 


18.65 


19.45 


26918.890 


0.637235? 




58 


-r 


14.8 


+ 


16.2 


18.85 


19.45 


26920.735 


0.514982 


Alt 0.525 


59 


+ 


26.2 


+ 


9.6 


18.55 


19.50 


35657.875 


0.463454 


Alt 0.480 


60 


- 


10.9 


+ 


7.7 


18.85: 


19.50 








61 


^ 


36.2 


+ 


18.8 


18.45 


19.50 


26918.865 


0.589141 




62 


- 


21.6 


+ 


3.0 


18.75 


19.55 


26975.650 


0.495233 




63 


+ 


14.1 


+ 


22.2 


18.65 


19.50 


27274.860 


0.527996? 





68 



Variable Stars in Globular Clusters 



No. 




x" 




y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC 7006 (continued) 














64 


+ 


21.4 


+ 


6.2 


18.80 


19.45 








65 


- 


8.7 


+ 


9.9 


18.70 


19.50 


36376.920 


0.544081 


Alt 0.515 


66 


+ 


28.1 


- 


2.5 


18.75 


19.50 


26918.730 


0.617159 


Alt 0.603 


67 


- 


14.1 


- 


1.1 


18.85 


19.45 








68 


+ 


12.7 


+ 


5.8 


18.60 


19.50 








69 


+ 


10.0 


+ 


3.9 


18.90: 


19.30: 








70 


-r 


8.7 




0.0 


18.40 


18.85: 








71 


- 


3.2 


- 


13.6 


18.80 


19.40 








72 


+ 


26.0 


- 


0.5 


18.80 


19.40 


26919.675 


0.2610439 


Alt 0.318 


73 


- 


15.5 




0.0 


18.40 


19.30 


35456.600 


0.577966 




74 


+ 


1.2 


- 


10.8 


18.40 


19.60 


27033.635 


0.566850 




75 


+ 


152.2 


1 


56.7 


18.40 


19.00: 


27300.600 


0.518750 





New vars. 44-52 Rosino and Mannino, 53, 54, Sandage and Wildey, 55-75 Rosino and Ciatti. 

Saiidage, ASP 66.324 (p) (1954); Rosino and Mannino, Asiago Contr 59 (p) (1955); Mannino, 
Asiago Contr 84 (1957); Rosino and Ciatti, Asiago Contr 199 (p) (1967); Sandage and WUdey, 
ApJ 150.469 (p) (1967); Pinto, Priv comm (1972) 

S55a, S57, S59, 861, R62a, S62, L65, R65, S67, S69, S70 



NGC 7078 (Messier 


15) a2lh27m.6. 


5+ll°57' 








1 


-118.6 


+ 24.4 


14.48 


15.52 


20724.394 


1.437523 


+, Sp 


2 


-171.7 


+ 6.0 


15.44 


16.00 


40442.58 


0.6842736 




3 


-248.0 


- 46.8 


15.70 


16.29 


40072.500 


0.3887407 




4 


-112.6 


-163.6 


15.58 


16.24 


40442.553 


0.3135758 




5 


-100.3 


-212.5 


15.66 


16.24 


40442.510 


0.3842142 




6 


+ 24.4 


+ 76.5 


14.93 


15.68 


25900.190 


0.6659671 




7 


+ 10.1 


+ 73.2 


15.56 


15.98 


25900.102 


0.3675643 




8 


- 0.6 


+ 126.8 


15.18 


16.01 


20725.103 


0.6462446 




9 


+ 15.6 


+ 138.7 


15.18 


16.09 


20724.993 


0.7152819 




10 


-1-125.6 


+ 1.7 


15.61 


16.18 


20724.967 


0.3863931 




11 


+ 172.3 


- 21.8 


15.52 


16.22 


20725.008 


0.3432527 




12 


-1-163.0 


- 50.7 


15.35 


16.12 


20724.930 


0.5928844 


BC 


13 


+ 126.6 


- 68.8 


15.25 


16.36 


20725.068 


0.5749536 




14 


+ 84.1 


-256.2 


15.76 


16.35 


20725.167 


0.3820024 




15 


+ 81.7 


-304.1 


15.26 


16.50 


20724.991 


0.5835687 


Be 


16 


+ 101.9 


+ 129.8 


15.50 


15.97 








17 


+ 83.7 


+ 110.6 


15.62 


16.17 


20725.001 


0.4288924 


+, B2 


18 


+ 77.3 


+ 100.4 


15.47 


16.05 


20725.101 


0.3677379 




19 


+ 111.3 


+ 160.4 


15.11 


16.42 


20725.038 


0.5723030 


Be 


20 


+ 81.2 


- 9.8 


15.04 


16.07 


25900.236 


0.6969598 




21 


+ 34.4 


- 57.5 


15.25 


16.20 








22 


-330.8 


- 45.8 


15.35 


16.36 


20724.719 


0.7201510 




23 


+ 192.0 


+ 256.1 


15.53 


16.33 


20724.891 


0.6326959 


Sp, BC 


24 


106.7 


- 6.1 


15.38 


15.96 


25900.534 


0.3696955 




25 


+ 302.9 


- 10.7 


15.49 


16.52 


20724.674 


0.6653286 




26 


+ 23.5 


+ 331.9 


15.83 


16.37 


20725.058 


0.4022695 


- 


27 


+ 222.5 


+ 248.2 


not var 











Catalogue 



69 



No. 


x" 


y" 


Max. 


Min. 


Epoch 


Period Remarks 


NGC 7078 (continued) 










28 


+ 309.9 


+ 534.2 


15.53 


16.53 


20724.739 


0.6706464 


29 


+ 163.3 


+ 212.2 


15.52 


16.37 


20725.128 


0.5749761 + 


30 


-165.0 


- 3.4 


15.55 


16.01 


40442.479 


0.4059796 BC 


31 


-112.6 


+ 245.6 


15.74 


16.30 


20725.044 


0.4081781 


32 


- 50.4 


+ 107.8 


15.01 


15.93 


25900.589 


0.6054003 


33 


- 41.2 


29.4 


15.15 


15.95 


24409.065 


0.5839452 


34 


- 55.4 


- 54.5 


prob vai 








35 


- 34.0 


-163.6 


15.70 


16.32 


20725.143 


0.3839986 


36 


- 27.7 


81.6 


15.12 


16.31 


25900.141 


0.6241424 


37 


- 25.2 


- 77.4 










38 


^ 7.6 


-146.2 


15.47 


16.09 


20725.100 


0.3752769 


39 


+ 20.5 


-124.8 


15.58 


15.98 


20725.184 


0.3895696 Be 


40 


+ 131.8 


-116.7 


15.46 


16.32 


20724.834 


0.3773302 


41 


+ 62.9 


- 55.4 


15.50 


16.15 


24409.010 


0.6452282 


42 


+ 227.5 


- 36.8 


15.68 


16.36 


20725.086 


0.3601745 


43 


+416.7 


+ 103.2 


15.74 


16.40 


20725.808 


0.3959928 


44 


+ 91.3 


+ 3.0 


15.00 


16.02 


20725.128 


0.5955547 - 


45 


+ 66.9 


- 31.0 


15.20 


16.15 


24409.224 


0.6773992 


46 


+ 56.0 


+ 33.2 


15.40 


16.32 






47 


+ 45.7 


- 4.3 


15.0 


16.2 


25900.380 


0.602799 


48 


+ 59.7 


+ 150.6 


15.4 


15.9 


25900.346 


0.3649762 


49 


+ 40.3 


+ 166.6 


14.83 


15.42 




0.6552054 


50 


+ 165.0 


+ 100.0 


15.52 


16.12 


25900.173 


0.2980583 + 


51 


+ 6.2 


+ 91.4 


15.56 


16.10 


25900.280 


0.3969565 


52 


+ 192.4 


- 22.6 


15.36 


16.44 


20724.800 


0.5756132 + 


53 


- 92.6 


-111.0 


15.60 


16.07 


20725.202 


0.4141270 


54 


+ 10.8 


+ 88.4 


15.55 


16.05 


25900.078 


0.3995683 


55 


+ 65.3 


- 18.8 


15.49 


16.30 






56 


+ 57.4 


0.0 


15.19 


16.11 






57 


+ 75.2 


- 56.4 


15.51 


16.06 


20724.891 


0.3492988 


58 


- 55.6 


+ 8.8 


15.5: 


16.10 






59 


+ 41.3 


+ 41.5 


15.10 


15.95 


24409.520 


0.5547922 


60 


+ 53.4 


- 59.3 


15.29 


16.00 






61 


- 67.3 


- 40.2 


15.2: 


15.8: 






62 


- 71.6 


+ 39.6 


15.3: 


15.8: 




0.3882: 


63 


+ 49.8 


+ 31.0 


15.54 


16.44 






64 


- 46.2 


+ 19.1 


15.5 


16.0 


25900.211 


0.355624 


65 


-102.4 


- 38.7 


15.55 


16.05 


24409.366 


0.7183491: 


66 


- 68.4 


-112.4 


15.61 


16.13 


20725.179 


0.3793488 


67 


- 86.6 


- 10.4 


15.5: 


16.2: 






68 


- 31.8 


+ 12.6 










69 


- 37.0 


- 25.2 










70 


- 34.0 


- 19.2 










71 


- 34.8 


- 12.6 










72 


- 2.2 


+ 34.8 


15.0: 


15.8: 


24409.042 


1.1386: 


73 


- 3.7 


+ 20.0 










74 


+ 36.3 


- 85.8 


15.45 


16.30 


24409.188 


0.296071 


75 


+ 2.2 


- 30.3 











70 



Variable Stars in Globular Clusters 



No. 




x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC 7078 (conti 


nued) 












76 


+ 


0.7 


- 28.9 












77 


- 


11.8 


- 22.9 












78 


- 


6.7 


+ 47.4 


15.15 


15.8: 


24409.421 


0.398879 




79 


+ 


21.5 


- 23.7 












80 


- 


47.4 


- 26.6 


15.1: 


15.8: 








81 


- 


21.5 


- 5.9 












82 


- 


20.7 


+ 1.5 












83 


+ 


16.3 


- 7.4 












84 


+ 


18.5 


- 16.3 












85 


+ 


20.7 


+ 2.2 












86 


+ 


12.6 


+ 4.4 


13.9 


14.8 


24410.62 


17.109 




87 


+ 


23.7 


- 23.7 












88 


+ 


2.2 


+ 26.6 












89 


- 


23.7 


- 6.7 












90 


+ 


31.1 


+ 4.4 












91 


+ 


67.3 


+ 28.9 


15.3: 


16.0: 








92 


+ 


9.6 


- 25.2 












93 


+ 


27.4 


- 33.3 


15.5: 


16.0: 








94 


+ 


3.7 


+ 28.9 












95 


+ 


5.2 


- 40.0 












96 


+ 


165.6 


+ 215.0 


15.85 


16.30 


24409.242 


0.396046 




97 


— 


79.5 


+ 29.3 


15.50 


16.25 


24409.548 


0.696333 




98 


- 


67.1 


+ 46.1 


15.4: 


15.95 


24409.07 


0.4701: 




99 


+ 


29.2 


+ 195.4 


15.70 


16.10 


24410.435 


0.277995: 




100 


+ 


12.5 


- 35.8 


15.5 


16.3 


24409.058 


0.406114 




101 


- 


104 


+ 540 


15.75 


16.30 


24409.292 


0.400360 




102 


+ 


68.8 


+ 31.5 


15.70 


16.15 


24409.119 


0.7589: 




103 


- 


251.5 


-273.3 


15.7 


16.4 


36070.16 


0.368126 




104 


- 


151.6 


-642.5 


15.6 


16.4 


36070.22 


0.414124 




105 


-: 


376.4 


-737.3 


15.6 


17.1 


36070.11 


0.571155 


f 


106 


- 


30.3 


+ 12.8 


15.5 


16.0 






RRc 


107 


- 


32.5 


- 21.8 


15.5 


15.9 






RRc 


108 


- 


32.4 


- 51.1 


15.5 


15.9 






RRc 


109 


+ 


12.7 


- 31.3 


15.5 


16.1 






RRc 


110 


+ 


31.7 


- 37.4 


15.5 


16.0 






RRc 


111 


+ 


41.7 


- 0.7 


15.3 


16.2 






RR 


112 


+ 


55.5 


+ 35.0 


15.3 


16.3 






RR 



New vars. 96-98 Izsak, 99 Mannino, 100-102 Notni and Oleak, 103-105 Tsoo Yu-hua, 106-112 
Rosino. Three of the corona stars of Kurochkin (1963) are similar to cluster members. 

Izsak, Budapest Mitt 28 (1952); Arp. AJ 60.1 (1955); Kholopov, VS 10.253 (1955); Grubissich, 
Asiago Contr 76 (1956); Mannino, Asiago Contr 74, 75 (1956); Izsak, Budapest Mitt 42.63 (1957); 
Nobili, Asiago Contr 81 (1957); Notni and Oleak, AN 284.49 (1958); Bachmann, AN 284.191 
(1958); Mannino, Asiago Contr 110 (1959); Bronkalla. AN 285.181 (1960); Preston, ApJ 134.651 
(1961); Yu-hua, Acta Astr Sinica 9.65 (1961); Fritze, AN 287.79 (1963); Kurochkin, VS 14.457 
(1963); Makarova and Akimova, VS 15.350 (1965); Rosino, IBVS 327 (1969); Mironov, AC 637.1 
(1971); Barlai, Priv comm (1972) 
S55a, S57. S59, S61, A62, R62a, S62, P64, S64, L65, R65, St66, S67, C&S69, S69, S70 



Catalogue 



71 



No. 


x" 


y" 


Max. 


Min. 


Epoch 


Period 


Remarks 


NGC 7089 (Messier 


2) a21 


Ii30m.9, 5 


-01°03' 








1 


+ 25.6 


+ 79.4 


13.2 


14.8 


26607.800 


15.583 


SpF-G 


2 


- 45.8 


+ 71.1 


14.6 


16.1 


21454.971 


0.527858 




3 


+ 222.9 


- 39.6 


15.1 


16.4 


26921.952 


0.6197006 




4 


- 26.8 


+ 31.5 


15.2 


16.6 


26628.644 


0.564247 




5 


- 44.4 


+ 2.1 


13.2 


14.9 


26628.644 


17.606 


SpF-G 


6 


+ 11.8 


- 45.4 


13.2 


14.9 


22162.928 


19.295 


SpF-G 


7 


+ 153.0 


-189.2 


15.1 


16.4 


27274.901 


0.594609 




8 


- 66.9 


- 56.8 


15.1 


16.4 


27273.896 


0.643677 




9 


-173.2 


-128.2 


15.2 


16.4 


27274.901 


0.609291 




10 


+ 90.6 


+ 38.8 


15.2 


16.4 


27275.909 


0.466910 


Sp 


11 


+ 85 


+ 8 


12.5 


14.0 


31259.8 


67.0 


Sp F-G, Min 


12 


- 62 


+ 43 


15.1 


16.5 


26628.776 


0.665616 




13 


- 77 


+ 73 


15.1 


16.4 


26924.972 


0.706616 




14 


+ 83 


- 68 


15.4 


16.4 


20749.843 


0.693785 




15 


+ 80 


- 76 


15.7 


16.4 


26944.880 


0.430152 




16 


- 31 


- 27 


15.3 


16.5 


27275.950 


0.655917 




17 


+ 2 


- 63 


15.2 


16.3 


27274.901 


0.636434 




18 


-189 


-707 


15.95 


16.85 


40088.467 


0.36226 


Pvar 


19 


+235 


-502 


16.00 


17.05 


39089.384 


0.319403 


P var 


20 


+400 


+ 74 


16.00 


16.75 


37162.281 


0.2863224 




21 


+ 315 


+ 208 


15.75 


16.85 


39789.516 


0.712178 


Pvar 



New vars. 18-21, Margoni and Stagni. 

Arp, AJ 60.1 (1955); Arp and Wallerstein, AJ 61.272 (1956); Wailerstein, AJ 62.168(1957), 
ApJ 127.583 (1958); Kulikov,VS 13.400 (1961); Mantegazza, Bologna Pubbl 8, 5 (1961); Preston, 
Krzeminski and Smak, ApJ 137.401 (p) (1963); Margoni and Stagni, IBVS 239 (1967); Kukarkin, 
IBVS253, 254(1968); Poole, Master's Thesis, Toronto (1968); Demers, AJ 74.925 (1969); Mar- 
goni and Stagni, Asiago Contr 213 (1969); Kukarkin, IBVS 422 (1970); Voroshilov, AC 623.7 
(1971); Eggen, ApJ 172.639 (1972) 
S55a, S57, S59, S61, R62a, S62, P64. S64, R65, S67, C&S69, S69, S70 



NGC 7099 (Messier 


30) a 2; 


lh37m.5. 


6-23°25' 








1 


+ 30.0 


- 60.6 


15.0 


16.5 


32060.525 


0.743608 




2 


+ 58.6 


-126.2 


14.92 


16.04 


32060.46 


0.65 35049 




3 


- 96.7 


- 39.6 


14.91 


16.06 


32039.59 


0.69632 




4 


-339: 


- 51: 


16.1 


[18 


32450 


9-10 


UG 


5 














Terzan 1 


6 














Terzan 2 


7 














Terzan 3 


8 














Terzan 4 


9 














Terzan 5 


10 














Terzan 6 


11 














Terzan 7 


12 














Terzan 8 



72 



Variable Stars in Globular Clusters 



No. 



y 



Max. 



Min. 



Epoch 



Period 



Remarks 



NGC 7099 (continued) 

Variables of Terzan (1968) identified on print. 

Rosino, Asiago Contr 117 (1961); Terzan, Haute Prov Publ 9, 24 (p) (1968); Dickens, Preprint 
(1972) 

S55a, R57, S57, S59, R62a, S62, S64, R65, St66, S69, S70 



Palomar 12 a2lh43m.7, 5 -21°28' 

Zwicky, RR 
RR, K&R 
103a-D plate K&R 

Zwicky, Morphological Astronomy, p. 205 (p) (1957); Kinman and Rosino, ASP 74.503 (p) (1962) 
R61,S61, S64,S69 



1 


-97.4 


+ 129.8 


20.3 


21.1 


2 


-80.8 


+ 136.8 


20.3 


21.5 


3 


-51.2 


+ 102.0 


18.5 


22 



Palomar 13 a 23h04m.2, 5 +12° 28' 



P var 



All four new variables, Rosino 

Rosino, Asiago Contr 85 (p) (1957); Ciatti, Rosino and Sussi, Bamb Kl Veroff 4, 40.228 (1965) 

R57, S59, R61, S61, S62, S67, S69 



1 


-32 


+ 32 


17.35 


18.55 


35759.505 


0.538158 


2 


+ 11 


- 10 


17.45 


18.60 


35782.381 


0.597111 


3 


- 8 


+ 21 


17.35 


18.55 


36455.770 


0.578168 


4 


+76 


-300 


17.55 


18.65 


35721.615 


0.575340 



NGC 7492 a23^05"i.7. 5 -15°54' 



+ 19.5 
-19.5 
+ 30.0 
-36.5 



+ 96.0 
+ 49.5 
-253.5 
-116.0 



17.07 
16.91 
17.39 



17.67 
17.31 
17.79 



37499.603 



15.66 15.96 



0.804873 
0.292045 
0.270998 
17.9 



red 



Three suspected variables, Barnes (1968), who found variables 2-4. 

Kinman and Rosino, ASP 74.503 (1962); Barnes, Priv comm (1966), AJ 72.291 (1967), AJ 
73.579(1968) 

S55a, S57, S59, S61, S62, 864, S67, S69, S70 



73 



INDEX OF ABBREVIATIONS USED IN REFERENCES, 
LISTED CHRONOLOGICALLY 



S55a Sawyer, H., Toronto Publ 2, 2: A Second Catalogue of Variable Stars in Globular Clusters, 

Table II. Summary of Variable Stars in 72 Globular Clusters (1955) 
S55b Sawyer, H., Toronto Publ 2, 2: Table I, Thirty-Four Globular Clusters Not Searched for 

Variables (1955) 
R57 Rosino, L., Budapest Mitt 42: Problems of Variable Stars in Globular Clusters (1957) 

S57 Sawyer Hogg, H., lAU Trans 9.548, Table 3a: Fifty-Nine Globular Clusters (1957) 

S59 Sawyer Hogg, H., Handbuch der Physik, ed. S. Fliigge (Berlin: Springer Verlag), p. 181 ; 

Star Clusters (1959) 
R61 Rosino, L., lAU Trans 118.300: Work Being Carried Out at the Asiago Observatory 

(1962) 

561 Sawyer Hogg, H., lAU Trans I1A.271: Report of Sub-Commission 27b, Variable Stars in 

Clusters (1962) 
A62 Arp, H.C., Symposium on Stellar Evolution, 1960, La Plata (1962) 

R62a Rosino, L., Pad Com 29, Tables 3 and 4: Clusters Observed for Variables (1962) 
R62b Rosino, L., Pad Com 29, Table 1: Clusters Never Observed for Variables (1962) 
R62c Rosino, L, Pad Com 29, Table 2: Clusters Insufficiently Observed for Variables (1962) 

562 Sawyer Hogg, H., Bamb Kl Veroff 34.8: Numbers and Kinds of Variables in Globular 

Clusters (1962) 
F&L63 Fourcade, C. R., and Laborde, J. R., La Plata Bol 6. 1 1 1 : Estrellas variables en cumulos 

globu lares (1963) 
P64 Preston, G., Ann Rev Astr Ap 2.23: The RR Lyrae Stars (1964) 

S64 Sawyer Hogg, H., lAU Trans 12A.390: Variable Stars in Star Clusters (1965) 

L65 Lohmann, W., AN 289.99; Perioden-Helligkeils-Beziehungen von RR Lyrae-Sternen in 

Kugelformigen Sternhaufen (1965) 
R65 Rosino, L., Bamb Kl Veroff 4.40.98: Characteristics and .'\bsolute Magnitudes of the RR 

Lyrae Variables in Globular Clusters (1965) 
FLA66 Fourcade, C. R., Laborde, J. R., and Albarracin, J., Atlas y Catalogo de estrellas variables 

en cumulos globulares al sur de -29°, Cordoba (1966) 
St66 Stothers, R., AJ 71.943: The Ultraviolet Dwarfs: A New Class of Degenerate Stars (1966) 

S67 Sawyer Hogg, H., lAU Trans 13A.555: Report of the Committee on Variable Stars in Clus- 

ters (1967) 
C&S69 Coutts, C, and Sawyer Hogg, H., Toronto Publ 3. 1 : Period Changes of RR Lyrae Variables 

in the Globular Cluster Messier 5 (1969) 

569 Sawyer Hogg, H., Non-Periodic Phenomena in Variable Stars, ed. L. Detre, p. 475: The 

Third Catalogue of Variable Stars in Globular Clusters (1969) 

570 Sawyer Hogg, H., lAU Trans i4A.291: Report of the Committee on Variable Stars in 

Clusters (1970) 
F72 Feast, M., Preprint: Red Variables in Globular Clusters, in the Galactic Centre and in the 

Solar Neighbourhood (1972) 



74 



INDEX OF ABBREVIATIONS OF PUBLICATIONS 



AAS Bull 
AAVSO Abstr 
AC 

Acta Astr Sinica 

AG Mitt 

AJ 

AN 

Ann Aph 

Ann Rev Astr Ap 

ApJ 

ApJ Suppl 

Asiago Contr 

ASP 

Astr Abh HolTmeister 

Astr and Ap 

BAC 

Bamb Kl Vcroff 

Bamb Veroff 

BAN 

BAN Suppl 

Berg Abh 
Bologna Pubbl 
Budapest Mitt 

Cordoba Repr 

HA 

Haute Prov Pub! 

HB 

HC 

lAU Coll 

lAU Draft Reports 

lAU Trans 

IBVS 

Inf Bull So Hemis 

JRASC 
JO 

La Plata Bol 
La Plata Symp 
Lea tie t 

Leiden Ann 



Bulletin of the American Astronomical Society 

Abstract of the American Association of Variable Star Observers 

Astronomical Circular. Bureau of Astronomical Information of the Academy 

of Sciences of USSR, Moscow 
Acta Astronomica Sinica 
Mitteilungen der Astronomischen Gesellschaft 

The Astronomical Journal. Published by the American Astronomical Society 
Astronomische Nachrichten. Akademic-Verlag, Berlin 
Annales d'Astrophysique. Revue Internationale trimestrielle 
Annual Review of Astronomy and Astrophysics. Palo Alto 
The Astrophysical Journal, An International Review of Spectroscopy and 

Astronomical Physics, Chicago 
The Astrophy.sical Journal. Supplement Series 

Contributi dell' Osservatorio Astrofisico dell" Universita di Padova in Asiago 
Publications of the Astronomical Society of the Pacific. San Francisco 
Astronomische .Abhandlungen Prof. Dr. C. Hoffmoister zum 70. Gcburtstag 

Gewidmet. Leipzig 
Astronomy and Astrophysics 

Bulletin of the Astronomical Institutes of Czechoslovakia. Prague 
Kleine Veroffentlichungen der Remeis-Sternwarte zu Bamberg 
Veroffentlichungen der Remeis-Sternwarte zu Bamberg 
Bulletin of the Astronomical Institutes of the Netherlands. Haarlem 
Bulletin of the Astronomical Institutes of the Netherlands. Supplement 

Series 
Abhandlungen aus der Hamburger Sternwarte. Hamburg-Bergedorf 
Pubblicazzioni deir Osservatorio astronomico univcrsitario di Bologna 
Mitteilungen der Konkoly-Sternwarte zu Budapest-Svabhegy 

Ob.servatorio de Cordoba. Reprint Series 

Annals of the Astronomical Observatory of Harvard College. Cambridge, 

I'SA 
Publications de TObservatoire de Haute Provence 
Bulletin of the Harvard College Observatory. Cambridge, L'SA 
Harvard College Observatory. Circular. Cambridge. US.A 

International Astronomical Union, Colloquium 
International Astronomical Union. Agenda and Draft Reports 
Transactions of the International Astronomical Union 
Information Bulletin on Variable Stars of Commission 27 of the Inter- 
national Astronomical Union. Budapest 
Information Bulletin for the Southern Hemisphere. La Plata 

The Journal of the Royal Astronomical Society of Canada 
Journal des Observateurs. Marseilles 

Asociacion Argentina de Astronomia. Boletin. La Plata 

Symposium on Stellar Lvolution, 1960. La Plata 

Publications of the .Astronomical Society of the Pacific. Leaflet. San I-ran- 

cisco 
Annalen van de Sterrewacht te Leiden 



75 



Louv Publ 

Lyon Publ 

MN 

Mt Wils Contr 

MVS 

NASA Tech Tr 

Obs 

Pad Com 

Proc Astr Soc Aust 

Pulk Mitt (Isw) 

Quart JRAS 

RAJ 

Royal Obs Ann 
Royal Obs Bull 

Rutherturd Contr 

SAI 

Sky Tel 
Sonn VerotT 
Soviet Astr AJ 



Spec Vat Ric 
Toronto Comm 

Toronto Pub! 

uoc 

VS 

VS Supp 

ZAp 



Publications du Laboratoire d' Astronomic et de Geodesic de I'Universite de 

Louvain 
Publications de I'Observatoire de Lyon. Serie I. Astronomic 

Monthly Notices of the Royal Astronomical Society. London 
Contributions from the Mount Wilson Observatory 

Mitteilungen iiber veranderliche Sterne. Herausgegeben von der Sternwarte 
Sonneberg 

National Aeronautics and Space Administration, USA. Technical Translation 

The Observatory. Monthly Review of Astronomy. Oxford 

Osservatorio Astronomico di Padova. Comunicazioni 
Proceedings of the Astronomical Society of Australia. Sydney 
Mitteilungen (Istvvestija) der russischen Hauptsternwarte zu Pulkovo 

The Quarterly Journal of the Royal Astronomical Society 

Russian Astronomical Journal (until 1931 ). .'Astronomical Journal of Soviet 

Union 
Royal Observatory Annals. Herstmonceu.x; Royal Greenwich Observatory 
Royal Observatory Bulletins. Joint Publications of the Royal Greenwich 

Observatory, Herstmonceux: Royal Observatory, Cape of Good Hope 
Contributions from the Rutherfurd Observatory of Columbia University, 

New York 

Memorie della Societa Astronomica Italiana 

Sky and Telescope. Harvard College Observatory, Cambridge. VS.\ 

Veroffentlichungen der Sternwarte zu Sonneberg 

Soviet Astronomy AJ. A translation of the Astronomical Journal of the 

Academy of Sciences of USSR. Published by the .American Institute of 

Physics, Inc., New York 
Specola Astronomica Vaticana. Richcrche .Astronomiche 

Communications from the David Dunlap Observatory, University of 

Toronto 
Publications of the David Dunlap Observatory, University of Toronto 

Circular of the Union Observatory 

Variable Stars. Academy of Sciences of USSR, Moscow 
Variable Stars. Supplement Series. Moscow 

Zeitschrift fur .Astrophysik. Berlin -Gottingen- Heidelberg 



PUBLICATIONS OF 

THE DAVID DUNLAP OBSERVATORY 

UNIVERSITY OF TORONTO 

Volume 3 Number 7 



THE SCULPTOR DWARF SPHEROIDAL GALAXY 

I. DISCOVERY AND IDENTIFICATION 
OF VARIABLE STARS 



by 
S.L. TH. J. VAN AGT 



1978 
TORONTO, CANADA 



PUBLICATIONS OF 

THE DAVID DUNLAP OBSERVATORY 

UNIVERSITY OF TORONTO 

VOLUME 3 Number i 



THE SCULPTOR DWARF SPHEROIDAL GALAXY 

I. DISCOVERY AND IDENTIFICATION 
OF VARIABLE STARS 



by 
S.L. TH. J. VAN AGT 



1978 
TORONTO, CANADA 



PRINTED AT 
UNIVERSITY OF TORONTO PRESS 



THE SCULPTOR DWARF SPHEROIDAL GALAXY 

L DISCOVERY AND IDENTIFICATION 

OF VARIABLE STARS 

S.L. Th. J. Van Agt 



Abstract 

All 602 variable stars in the Sculptor dwarf spheroidal galaxy which have been discovered by 
the author and by previous investigators are identified. Positions are given in rectangular coordi- 
nates relative to the center of the distribution of the variables at RA (1950) = 0^57"M4^ ± 2^, 
Dec (1950) = 34°0'23"±20". 

For 64 variables preliminary periods are given. 

The estimated total number of variables in the Sculptor gala.xy is 1050 ± 80. 



Introduction 

The discovery of the dwarf galaxy in Sculptor by Harlow Shapley (1938 a) and the 
subsequent discovery of a similar object in Fornax (Shapley 1938 b) came when the 
interest of astronomers was focussed strongly on the significance of the sequence of 
galactic forms. They consequently attracted considerable interest. 

In the Local Group ten Sculptor-type galaxies are now known. Table 1 includes the 
recently discovered dwarf spheroidal galaxy in Carina (Cannon, Hawarden and Tritton 
1977). 

TABLE I 
Sculptor-Type Galaxies 



Name 




1 


b 


Remarks 


Fornax 




237" 


-66" 


Shapley (1938 a) 


Sculptor 




286 


-83 


Shapley (1938 b) 


Leo I 




226 


+ 49 


Wilson (1955) 


Leo II 




219 


+ 67 


WUson (1955) 


Ursa Minor 




103 


+ 45 


Wilson (1955) 


Draco 




86 


+ 35 


WUson (1955) 


Carina 




260 


-22 


Cannon etal (1977) 


Andromeda 


I 


122 


-25 


van den Bergh (1972) 


Andromeda 


II 


129 


-29 


van den Bergh (1972) 


Andromeda 


III 


119 


- 26 


van den Bergh (1972) 



Nowadays the study of the dwarf spheroidal galaxies, especially of those nearest to 
us, contributes to investigations of stellar evolution and the evolution of the Local 
Group. (Norris and Zinn 1975, Lynden Bell 1976, Mathewson and Schwarz 1976). 
However knowledge about the stellar content and more specifically the numerous 
variable stars is still incomplete for these systems, as shown in review papers about the 
dwarf spheroidals by van den Bergh (1968, 1975), van Agt (1973) and Hodge (1971). 

This report is a first contribution in an extended study of the variable stars in the 
dwarf spheroidal galaxy in Sculptor. 



205 



206 Publications of the David Dunlap Observatory 

Distance And Dimensions 

Shapley (1938 a) assumed correctly, on the basis of his scanty preliminary data, 
that the stellar population of the Sculptor galaxy was in many respects comparable 
with that of galactic globular clusters. On the assumption that the brightest stars 
in the Sculptor galaxy would iiave an absolute photographic magnitude of about 
Mpg= 1.5, Shapley (1938a) derived a distance of 80 kpc. 

Baade and Hubble (1939) observed the Sculptor galaxy with the 100-inch Mount 
Wilson telescope and were the first to discover, on a small number of plates, two 
variables thouglit to be W Virginis stars and 38 RR Lyrae variables, the latter visible 
close to the plate limit and only when they were near maximum luminosity. 

On the basis of the observed mean maximum luminosity nip^ = + 19.12 for the 
RR Lyrae stars. Baade and Hubble (1939) derived a distance of 84 kpc for the Sculptor 
galaxy. For these stars they assumed a semi-amplitude of 0.5 mag. and a median abso- 
lute magnitude of M = 0.0 Later corrections to the sequence in SA 68 (Stebbins, 
Whitford, Jolmson 1950) used by Baade and Hubble for the transfer to Sculptor were 
balanced by the shift of the median absolute photographic magnitude for RR Lyrae 
stars to fainter values so that Baade and Hubble's value of the distance (Hodge 1965) 
remains almost unaltered. 

The two bright cepheids in Sculptor discovered by Baade and Hubble belong to a 
class of cepheids whose period-luminosity law differs from that of the cepheids in 
globular clusters (Baade and Swope 1961, van Agt 1973, van den Bergh 1975). Such 
anomalous cepheids with P<10 days are also found in other dwarf spheroidal galaxies 
of the Local Group and are brighter than the BL Herculis variables of population II 
with P less than 10 days in galactic globular clusters. Provisional periods for these 
anomalous BL Her variables in the Sculptor cluster were determined by Miss Swope 
(Shapley 1939) and used by Shapley for a new distance determination of 76 kpc. In 
view of the uncertainties involved, this result is in agreement with his earlier estimate 
(Shapley, 1938 a) and with the value derived by Baade and Hubble (1939). 

Hodge (1965) derived the first C-M diagram for the Sculptor dwarf spheroidal 
galaxy but it did not reach the horizontal branch. From the luminosities of the giant 
branch stars, the two anomalous BL Her stars, and the three RR Lyraes observed at 
maximum luminosity near the limit of his plates Hodge (1965) estimated a distance of 
88 ± 7 kpc. 

Kunkel and Demers (1977) recently derived a new distance of 78.3 kpc for Sculptor 
from the luminosity of the horizontal branch stars in the region of the variable gap in 
their C — M diagram. Their determination essentially confirms the results of the earlier 
investigators. 

The apparent diameter was first determined by Shapley (1938 a) from star counts. 
Shapley's observations indicate an apparent radius of at least 40 arcmin but they do 
not exclude a radius of as much as 60 arcmin. From star counts Hodge (1965) derived 
a limiting radius of 53 arcmin, a value consistent with Shapley's result. At the distance 
of 78.3 kpc Hodge's angular radius yields a linear diameter of 2.4 kpc. 

The variable stars reported on here extend up to distances from the center of the 
Sculptor galaxy of 60 — 70 arcmin. These values are in reasonable agreement with 
Shapley's conclusion that the Sculptor system might have a radius as large as 60 arcmin. 



The Sculptor Dwarf Spheroidal Galaxy 207 

The dwarf spheroidal galaxies have many characteristics in common with globular 
clusters and at the same time show remarkable differences (van den Bergh 1975, van 
Agt 1973). The dwarf spheroidal galaxies are obviously considerably larger, but so far 
no transitional object with respect to hnear dimension has been found. 



OBSERVATIONS 

Thackeray observed the Sculptor dwarf spheroidal galaxy during the observing sea- 
sons of 1948, 1949, 1950 and 1951 with the 74-inch Radchffe telescope. His aim was 
specifically to investigate and discover variable stars in the central part of the dwarf 
galaxy. The surface density of the stars in the central region is sufficiently low to per- 
mit resolution of individual stars. 

As a preUminary result Thackeray (1950) reported 237 variable stars and he derived 
provisional results on periods for 33 of them. He estimated the total number of varia- 
bles to be 700. Our investigation of the variable stars in the Sculptor dwarf galaxy is 
a continuation of Thackeray's survey and for this purpose Thackeray kindly put his 
plates and reductions at our disposal. Considering both the number of variable stars 
marked by Thackeray in the central part of the galaxy and the dimensions of the 
system a bountiful harvest of variable stars was expected from the outset of our 
investigation. 

In 1965 Sidney van den Bergh obtained a series of plates on the Sculptor system 
with the 48-inch Palomar Sclimidt. In 1970 Christine Coutts obtained additional obser- 
vations with the 24/36-inch Curtis Sclimidt of the University of Michigan installed at 
Cerro Tololo, Chile. Helen Sawyer Hogg started the blinking of these plates at the 
David Dunlap Observatory. This material was turned over to me when I arrived at that 
Observatory on leave from the Department of Astronomy at the Nijmegen University, 
the Netherlands. I continued the series of Curtis Schmidt plates at Cerro Tololo in 
1971. In addition Serge Demers put at our disposal the plates of Sculptor obtained by 
him with the same telescope in 1968 and 1969. 

The field of the Curtis Schmidt telescope is well suited for observations of an ex- 
tended object such as the Sculptor dwarf galaxy. On the plates taken with this tele- 
scope, which has a plate scale of 96'.'6/mm, inspection of the individual stars is possible 
even in the central region of this galaxy. This is due in part to the low surface density 
of stars and in part to the use of Kodak Illa-J emulsion which partly overcomes the 
limit to linear resolution set by the small plate scale. To reach sufficiently low Hmiting 
magnitudes the plates are typically exposed for two hours. This leads to a reduction of 
the resolution in time of the brightness variations, especially for the variables with the 
shortest periods. For the c-type RR Lyrae with periods between 5 and 1 1 hours the 
exposures integrate a considerable part of the light curve. Obviously there is a reduced 
possibility of detection of the shortest period variables as a consequence of the long 
exposure time. 

The photographic observations available to the author are listed in table II. They 
cover the period from 1938 to 1971. The earliest ones are the plates obtained by 
Baade (1939) and Hubble (1939). The large number of observations listed in table II 
provides a good time base for period determination. 



208 



Publications of the David Dwilap Observatory 



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The Sculptor Dwarf Spheroidal Galaxy 



209 



During the observing run of 1971 the author also obtained a small number of photo- 
graphic transfers to the sequences set up in Kron 3 (Walker 1970) and in NGC 121 
(Tifft 1963) to extend the sequencein the Sculptor dwarf galaxy that had been obtained 
by Hodge (1965) to fainter limits. Two such transfers were also obtained with the 60- 
inch telescope at Cerro Tololo and used for the same purpose (van Agt 1973). A com- 
parison of the photoelectric sequence of Kunkel and Demers (1977) and preliminary 
results from the photographic transfers does not show any serious discrepancies. 

DISCOVERY AND IDENTIFICATION 

From among the Curtis Schmidt plates available at the end of 1970 and listed in 
table III, selection of pairs for blinking was made on the basis of time interval, plate 
quality and Hmiting magnitude (table IV). The plate combinations were all blinked on 
the Zeiss bUnk comparator of the David Dunlap Observatory. The work was carried 
out without reference to preceding variable star searches by Baade and Hubble (1939), 
Thackeray (1950) and Helen Sawyer Hogg (1970). In all, 521 stars were marked by 
the author as variable or as being suspected of briglitness variations. 

The 602 variable stars discovered both by previous investigators and the author are 
listed in table V. They are numbered in chronological order of discovery. 

The variable stars numbered 1 through to 26 are those first found by Baade and 
Hubble (1939). Baade and Hubble identified (1939) only 10 variable stars out of the 
40 they discovered. On an unpublished chart of the Sculptor system Baade identified 



TABLE III 

List Of The 1969-1970 Curtis Schmidt Plates. 



CTIO Plate Nr. 


Date 






Exp. Time 


Emulsion 


Filter 


Remarks 


5084 


Sept 18 


1969 


120 min 


103aE 


NG 


2 




5166 


Oct 


12 


1969 


120 


IllaJ 


GG 


13 


baked plate 


5168 


Oct 


12 


1969 


120 


lllaJ 


GG 


13 


baked plate 


5176 


Oct 


13 


1969 


120 


IllaJ 


GG 


13 


baked plate 


5184 


Oct 


14 


1969 


120 


IllaJ 


GG 


13 


baked plate 


5186 


Oct 


14 


1969 


120 


IllaJ 


GG 


13 


baked plate 


5190 


Oct 


15 


1969 


120 


IllaJ 


GG 


13 


baked plate 


5197 


Oct 


16 


1969 


120 


IllaJ 


GG 


13 


baked plate 


5643 


Dec 


13 


1969 


90 


IllaJ 


GG 


13 


baked plate 


7093 


Aug 


4 


1970 


120 


IllaJ 


GG 


13 




7095 


Aug 


4 


1970 


120 


IllaJ 


GG 


13 




7111 


Aug 


6 


1970 


120 


IllaJ 


GG 


13 




7113 


Aug 


6 


1970 


120 


IllaJ 


GG 


13 




7128 


Aug 


7 


1970 


120 


IllaJ 


GG 


13 




7130 • 


Aug 


7 


1970 


120 


IllaJ 


GG 


13 




7142 


Aug 


8 


1970 


120 


IllaJ 


GG 


13 




7144 


Aug 


8 


1970 


120 


IllaJ 


GG 


13 




7161 


Aug 


9 


1970 


120 


IllaJ 


GG 


13 




7163 


Aug 


9 


1970 


120 


lllaJ 


GG 


13 




7180 


Aug 


10 


1970 


120 


IllaJ 


GG 


13 





2 1 Publications of the David Dunlap Observatory 

TABLE IV 

Plate Pairs Formed For Blinking 
From The 1969-1970 Curtis Schmidt Observations. 



Plate Pair Nr. 


CTIO Plate Nr. 


Time 


Interval 


1 


7093, 7180 


6^ 


.086 


2 


7130, 7163 


2 


.001 


3 


7093 , 7095 




.312 


4 


5166,5186 


2 


.126 


5 


5176,5184 


1 


.019 


6 


7093, 7163 


5 


.097 


7 


5168, 7130 


299 


.097 


8 


5166,7130 


299 


.232 


9 


5176,7130 


298 


.202 



16 more however. For the remaining variable stars reported by Baade and Hubble no 
identification could be traced. 

The variable stars numbered 27 through 241 are the ones newly discovered by 
Thackeray (1950) on the plates obtained with the Radcliffe telescope. These did not 
include plates off-set from the center of the dwarf galaxy. Variable stars farther from 
the center than approximately 20 arcmin therefore remained undetected. 

In the preliminary search for variables on the Curtis Schmidt plates Helen Sawyer 
Hogg discovered 49 new variable stars. These objects have been assigned the numbers 
242 through to 290. 

The remaining stars, numbered througli to 603, are the new variable stars discovered 
by the author. The star number 474 was subsequently found not to be a variable star 
and consequently has been eliminated from table IV. The total number of variable 
stars listed in table IV is therefore 602. 

Kunkel and Demers (1977) found from their photographic photometry that their 
star 213 shows widely discrepant magnitudes on both B and V plates. They suspected 
this star to be variable; it is identified by Kunkel and Demers (1977) in their figure 5 
as Star V. On the Radcliffe plates the photographic image of this object is in general 
not compatible with star images of similar photographic density. On recently obtained 
photographic observations at the prime focus of the 3.6 meter telescope of the European 
Southern Observatory at La Silla, Chile, this object under good seeing conditions is 
resolved as a faint galaxy. Widely varying magnitudes can be expected if such an object 
is mistaken for stellar and measured on plates obtained under not identical seeing 
conditions. 

The variable stars Hsted in table V are identified by their number on Plates I, II, III, 
IV, V and VI. On all these Plates, directions on the sky and the scale are indicated. 

The stars marked with "f ' in column 5 of table V are those farthest away from the 
center of the Sculptor galaxy and not within the area that is represented in plate VI. 



The Sculptor Dwarf Spheroidal Galaxy 2 1 1 

Center 

Counts have been made of all the variables listed in table V in strips 60" wide placed 
over the galaxy in the directions of right ascension and declination. The maxima of the 
counts in the strips orientated in this way led to the adopted position for the center of 
the distribution of the variable stars at RA (1950) = 0h57"M4s ± 2^ Dec (1950) = 
-34°0'23" ± 20". 

Coordinates Of The Varl^bles 

The coordinates were calculated from plate positions determined with the measuring 
facility of the projecting blink-comparator of the Department of Astronomy of the 
University of Nijmegen, the Netherlands (van Agt, 1972). The plate constants were 
derived from standard coordinates using a plate-scale of 96'.6/mm. 

The rectangular coordinates are given for each of the 602 stars in columns 2 and 3 
of table V. These coordinates are quoted in seconds of arc and are relative to the 
adopted center of the distribution of the variable stars. 

The accuracy in the x and y coordinates, corresponding respectively to right ascen- 
sion and declination, is ± 4 arcsec. 

Completeness 

The total number of discoveries of variable stars in a series of plate comparisons and 
the average number of times that each variable was found have been used by van Gent 
(1933) to derive the probability vv of discovering a variable star on each plate pair of 
the series and N, the total number of variable stars which can be expected to be present 
in the field investigated. In each of the nine intercomparisons, N was calculated by 
applying van Gent's method (van Gent, 1933, Plant, 1965, Hoffmeister 1970). The 
results are given in table VI. 



TABLE VI 

The Discovery Probability And Expected Number Of Variable Stars. 



Number of 


Discovery 


Tota: 


L of Variables 


Intercomparisons 


Probability w 


Expected N 




(van 


Gent 1933) 


(van 


Gent 1933) 


1 




- 




- 


2 




0.152 




650 


3 




0.160 




692 


4 




0.207 




631 


■ 5 




0.206 




682 


6 




0.182 




773 


7 




0.162 




805 


8 




0.141 




839 


9 




0.129 




897 



212 Publications of the David Dunlap Observatory 

There is a tendency for the discovery probability w to decrease as more and more 
plate pairs are intercompared. Hoffmeister (1933) pointed out that this decrease indi- 
cates the existence of a dispersion in the discovery probability among the variable stars. 
This dispersion is not taken into account in van Gent's method, which is based on the 
assumption that the discovery probability for each variable in the field is the same on 
each plate pair. There are a number of parameters to wiiich the discovery probability 
of a variable star can be related. The effects of the apparent brightness of the stars, 
the shape of tlie hglit curve and the range of the briglitness variations have been inves- 
tigated by a number of authors (Kviz 1956, Kiang 1962, Plaut 1953). Also variations 
in the quality of the plate pairs and changes in the attitude of the observer may cause 
variations. In a general way the decrease of the discovery probability can be explained 
by the fact that during the first intercomparisons those variables will be found which 
have large discovery probability and in later intercomparisons essentially those variables 
are left which have small discovery probability (Hoffmeister 1933). Of the variables 
discovered by Baade 92% were rediscovered. Of those found by Thackeray in liis exten- 
sive survey of the central region, 71% were rediscovered. 

Kviz (1959) and Kiang (1962) have pointed out that the net effect of not taking 
into account variations in the discovery probability is an overestimate of w and there- 
by an underestimate of N. Richter (1968) in an extension of van Gent's method found 
that for RR Lyrac variables the total number of variables N computed with van Gent's 
method should be increased by a factor of 1 .2 when one takes into account systematic 
effects on the discovery probability. From a semi-empirical method Plaut (1966) 
derived essentially the same factor. 

From the preliminary periods and the average median luminosities of the variables 
in Sculptor it is safe to conclude that most of the variables are RR Lyrae stars. In view 
of the Hmited data on the variable stars at this time it is not possible to analyse the 
blink statistics with either Richter's or Plant's method. For the time being we there- 
fore simply adopt Richter's factor of 1 .2 for extrapolating the results of table VI to 
obtain a somewhat more realistic total number of variables in the dwarfgalaxy of 1050, 
with an estimated mean error of 80. The low hnear resolution of the Curtis Schmidt 
plates in combination with the increased surface density of stars in the central region 
of Sculptor reduces the discovery probability relative to the outer regions of the system. 
The somewhat lower completeness factor derived from the number of rediscoveries of 
Thackeray's variables is not in disagreement with our completeness arguments. 

The RR LYRAE Stars 

At the present stage of the reductions, preliminary results on the periods for some 
of the variable stars are reported. In column 4 of table V periods for 64 stars are given. 
These periods have been determined by Thackeray and liis co-workers Jackson, Shuttle- 
worth and Wesselink, all of whom took part at certain stages in the reductions, and by 
the author. In column 5 of table V initials indicate to whom each period determination 
should be attributed. The variable stars for which periods have been determined are 
located in the central region of the dwarf galaxy because so far only the Radcliffe 
observations have been used for this. 



The Sculptor Dwarf Spheroidal Galaxy 2 1 3 

Among those with periods, 51 are ab-type RR Lyrae stars and 9 have c-type RR 
Lyrae star characteristics. Although it is expected that the shortest period c-type 
RR Lyrae are under-represented in the discoveries, due to the long exposure times of 
the observations, it is evident that c-type RR Lyrae stars in Sculptor are not as scarce 
as in the Draco dwarf galaxy where they number about 4% of the number of RR Lyrae 
stars, (Baade and Swope 1961). The frequency distribution of the periods of the RR 
Lyrae stars in the Sculptor galaxy is smooth, does not show double maxima and is in 
general very similar to the period-frequency diagram of the galactic globular cluster 
NGC 5272 (Messier 3), (van Agt 1973, Cacciari and Renzini 1976, Thackeray 1950). 

The mean period of the 51 ab-type RR Lyrae stars is P = 0^.567. The shortest 
period in this sample of ab-type RR Lyrae stars is P = 0'^.482 (V66) and the longest is 
P = 0'i.836(V88). 

The mean periods of the ab-type RR Lyrae stars in four dwarf spheroidal galaxies 
are listed in table Vli together with the number of ab-type RR Lyrae stars from which 
each mean period was determined. 

TABLE VII 
MEAN PERIODS OF ab-TYPE RR LYRAI: IN DWARF SPHEROIDAL GALAXIES 



Name P Number of ab-typc 



Sculptor 


o'l.se? 


51 


Draco 


.611 


126 


Ursa Minor 


.636 


21 


Leo II 


.592 


64 



Evidently the distribution of the mean periods of ab-type RR Lyrae stars in dwarf 
spheroidal galaxies does not follow the concept of the two period-groups observed for 
the RR Lyrae stars in galactic globular clusters by van Agt and Oosterhoff (1959). The 
mean period for the long period group (group I) is P = 0*^.647 ± 0.015 and for the 
short period group (group II) is P = 0'^.549 ± 0.010. 

The Anomalous BLHerculis Stars 

The variable stars V25 (= Baade-Hubble A), V26 (= Baade-Hubble B), and VI 19 be- 
long to the class of anomalous BL Her stars which also have been discovered in other 
dwarf spheroidal gslaxies in the Local Group (Swope 1968, Baade and Swope 1961, 
van Agt 1967). Similar variable stars are probably present in tiie Small Magellanic 
Cloud (van Agt 1973, Graham 1975). Zinn and Dahn (1976) report that V19 in the 
galactic globular cluster NGC 5466 might well belong to the class of anomalous BL 
Her stars, if indeed this variable is a member of the cluster. The anomalous BL Her 
stars are brighter by approximately 0.5-1 .0 m at the same period than the cepheids 
in the galactic globular clusters (van Agt 1973, Baade and Swope 1961. van den Bergh 
1975). 

Kunkel and Demers (1977) recently determined the photometric properties of the 
Baade-Hubble variable stars A and B (V25 and V26). They are located in the C M dia- 



214 Publications of the David Dunlap Obsen>atory 

gram of the Sculptor dwarf galaxy about 1 .4 mag above the horizontal branch and are 
about half a magnitude brighter than the population II cepheids in galactic globular 
clusters of the same period. 

Plates obtained recently at the prime focus of the 3.6 meter telescope of the 
European Southern Observatory show that V92, formerly classified as an anomalous 
BL Her star (van Agt 1973), is an optical double. One component is variable, the other 
is a star of similar mean luminosity. When unresolved, such an object would appear to 
have a luminosity in the range of the anomalous BL Her stars. 

On the basis of the presently available data Norris and Zinn (1975) and Demarque 
and Hirschfeld (1975) offer a hypothesis to explain the observed period-luminosity 
relation for the anomalous BL Her stars. They suggest that these stars belong to a 
younger population of stars than the majority in the same dwarf spheroidal galaxy, 
which itself was formed independently of and after the collapse of our galaxy. Renzini, 
Mengel and Sweigart (1977) suggest, however, that if higher masses are assumed for 
the anomalous BL Her stars, mass-transfer within binary systems in the dwarf spheroi- 
dal galaxies also is a hypothesis in agreement with the observational evidence. 

Long-Period and rfd-Irregular Variable Stars 

V544 located at about 14 arcmin north of the center of the Sculptor dwarf galaxy 
is bright on Curtis Schmidt plates taken in August 1970, but faint on plates taken in 
the same month one year earlier. Eye estimates of the variable star on the Radcliffe 
plates, where the star is in an unfavorable position close to the plate border, show the 
variable going througli a maximum in 1949. The time of rise to maximum and the time 
of decline to minimum is of the order of 120 days. A longer period of 150 days is 
possible. 

V97 is identical to the extremely red star numbered 453 in the list of Hodge (1965) 
of stars measured for the C M diagram. In his C-M diagram this variable star is located 
at B-V = 2.16 mag., toward the red of the brightest stars of the giant branch. Eye 
estimates indicate a range in luminosity of approximately 0.6 m V97 is not among 
the stars measured by Kunkel and Demers (1977). 

ACKNOWLEDGEMENTS 

I want to express my gratitude to the Director of the David Dunlap Observatory Dr. Donald 
A. MacRae, who made it possible for me to accept the kind invitation of Dr. Helen Sawyer Hogg 
and Dr. Sidney van den Bergh, to continue my work on the Sculptor dwarf spheroidal galaxy at 
their observatory under such pleasant conditions. To them in particular I direct my appreciation 
for their assistance and patience. 

The plates by Baade and Hubble were kindly put at my disposal by Dr. Horace W. Babcock. 
the Director of the Mount Wilson and Palomar Observatories. 

Without the cooperation of Dr. A.D. Thackeray who made the Radcliffe plates and his research 
notes available, this work would still lack the basic observations for the determination of periods. 

I appreciate the cooperation of the CTIO directorate and staff who helped in obtaining the 
excellent new Curtis Schmidt observations. 

To the staff of the David Dunlap Observatory and especially Dr. Christine Coutts-Clement I am 
indebted for their help and for their excellent observational material obtained at CTIO. I also want 
to thank Dr. Paul Hodge. Dr. Serge Demers and others who in many ways helped or are helping 
with the Sculptor project. 



The Sculptor Dwarf Spheroidal Galaxy 2 1 5 

The research was supported by grants to Professors Hogg and van den Bergh through the 
National Research Council of Canada, and by the David Dunlap Observatory. 

References 

Agt, S. van and Oosterhoff, P. 1959, Ann. Sterrew. Leiden, vol. 21, p. 253. 

Agt, S. van. 1972, Proc. Conf. on the Role of Schmidt Telescopes in Astronomy, ed. U Haug 

(Hamburg Obs.) p. 97. 
Agt, S. van. 1973, Variable Stars in Globular Clusters and in Related Systems, ed. J.D. Fernie 

(Dordrecht-Holland), p. 35. 
Baade, W. and Hubble. E. 1939. Publ. Astron. Soc. Pacific, vol. 57, p. 40. 
Baade \V. and Swope, H. 1961, Astron. J., vol. 66, p. 300. 
Bergh, S. van den. 1968. J. Roy. Astron. Soc. Canada, vol. 62, p. 145. 
Bergh. S. van den. 1972, Astroph. J. Letters, vol. 1 71, p. L31. 
Bergh, S. van den. 1975, Ann. Rev. Astron. Ap., vol. 13, p. 217. 
Cacciari, C. and Renzini. V. 1976, Astron. Astroph. Suppl., vol. 25, p. 303. 

Cannon, R., Hawarden, T. and Tritton, S. 1977, Monthly Notices Roy. Astron. Soc, vol. 180, p. 81. 
Demarque, P. and Hirschfeld, A.W. 1975, Astroph. J., vol. 202, p. 346. 
Gent, H. van. 1933, Bull. Astron. Inst. Neth., vol. 7, p. 21. 
Graham, J. 1975, Publ. Astron. Soc. Pacific, vol. 87, p. 641. 
Hodge, P.W. 1961, Astron. J., vol. 66, p. 384. 
Hodge, P.W. 1965, Astroph. J., vol. 142, p. 1390. 
Hodge, P.W. 1971, Ann. Rev. Astron. Astroph., vol. 9, p. 35. 
Hoffmeister, C. 1933, Astron. Nachr., vol. 250, p. 397. 
Hoffmeister, C. 1970, Veranderliche Sterne (Barth: Leipzig), p. 171. 
Kiang, T. 1962, Observatory, vol. 82, p. 57. 
Kunkel, W.E. and Demers, S. 1977, Astroph. J., vol. 214, p. 21. 
Kviz, Z. 1958, Bull. Astron. Inst. Czech., vol. 9, p. 70. 
Kviz, Z. I960, Bull. Astron. Inst. Czech., vol. 77, p. 71. 
Lynden-Bell, D. 1976, Monthly Notices Roy. Astron. Soc, vol. 7 74, p. 695. 

Mathewson, D.S. and Schwarz, M.P. 1976, Monthly Notices Roy. Astron. Soc, vol. 7 76, p. 47. 
Norris, J. and Zinn, R. 1975, Astroph. J., vol. 202, p. 335. 
Plaut, L. 1965, in Galactic Structure, eds. A.Blaauw and M. Schmidt, (University of Chicago Press: 

Chicago), p. 302. 
Plaut, L. 1953. Pub. Kapteyn Astron. Lab. Groningen, vol. 55. 
Plaut, L. 1966, Bull. Astron. Inst. Neth. Suppl., vol. 7, p. 105. 

Renzini, V., Mengel, J. and Svveigart, A. 1977, Bull Am. Astron. Soc, vol. 9, p. 279. 
Richter, G. 1968, Veroffentl. Sternwarte Sonneberg Berlin, band 7, heft 3. 
Sawyer Hogg, Helen 1970, private communication. 
Shapley, H. 1938 a. Harvard BuU., No. 908, 1. 
Shapley, H. 1938 b, Nature, vol. 142, p. 715. 
Shapley, H. 1939, Proc. Nat. Acad. Sci., vol. 25, p. 565. 

Stebbins, J., Whitford, A. and Johnson, H. 1950, Astroph. J., vol. 7 7 2, p. 469. 
Swope, H. 1968, Astron. J., vol. 73, p. S 204. 
Thackeray, A. 1950, Observatory, vol. 70, p. 144. 
Tifft, W. 1963, Monthly Notices Roy. Astron. Soc, vol. 726, p. 209. 
Walker, M. 1970, Astroph. J., vol. 767, p. 835. 
Wilson, A. 1955, Pub. Astron. Soc Pacific, vol. 67, p. 27. 
Zinn, R. and Dahn, C. 1976, Astron. J., vol. 81, p. 527. 

Nijmegen University 
August, 1977 



2 1 6 Piiblications of the David Dunlap Observatory 

TABLE V 

Variable Stars In The Sculptor Dwarf Spheroidal Galaxy: 

Coordinates And Preliminary Periods. 

NR X" Y" Period Remarks 



.d.i 



1 - 455. 184. P = "-532 Th 

2 - 413. 93. 

3 52. 410. 

4 - 250. 108. 

5 53. 72. P = ^-484 Th.vA 

6 - 91. - 150. 

7 191. 161. P='^-285: Th 

8 26. - 49. 

9 - 46. -211. 

10 43. -196. P = '^-515 vA 

11 46. -215. P = '^-561 vA 

12 251. -119. 

13 - 5. 640. P = '^-340 Th 

14 - 612. - 95. 

15 - 239. 280. 

16 10. 416. 

17 - 310. - 94. 

18 - 53. 139. 

19 145. 290. 

20 199. 53. 

21 155. - 134. 

22 - 52. -590. 

23 192. -440. 

24 363. - 282. 

25 - 94. 560. 

26 19 3. -276. 

27 1149. -102. 

28 1076. 183. 

29 897. 610. 

30 895. 600. 

31 778. 355. 

32 813. -456. 

33 728. 119. P = '^-343 vA 

34 702. -109. P = '^-662 vA 

35 699. - 95. P = '^-526 vA 

36 683. -474. P = '^-624 vA 

37 582. 237. 

38 556. 268. P = '^-502 vA 

39 578. - 84. P = '*-506 vA 

40 572. - 548. 

41 512. - 50. P = '^-547 vA 

42 503. 51. P = '^-596 vA 



P = '*-289 


vA 


P = '^-639 


Th 


P = ''-588 


vA 


P = '^-510 


Th 


P = S25 
P=l'^-35 


Baade A, Th, vA 


Baade B, Th, vA 



43 495. 75. P = '^-617 vA, J 

44 501. - 314. 

45 496. - 519, 

46 453. 117. 



The Sculptor Dwarf Spheroidal Galaxy 2 1 7 

TABLE V (continued) 

NR X" Y" Period Remarks 

47 
48 
49 
50 
51 
52 
53 
54 
55 
56 
57 
58 
59 
60 
61 
62 
63 
64 
65 
66 
67 
68 
69 
70 
71 
72 
73 
74 
75 
76 
77 
78 
79 
80 
81 
82 
83 
84 
85 
86 
87 
88 
89 
90 
91 



485. 


-483. 


P = '^-526 : 


Th 


472. 


-440. 


P = '^-565 


Th, vA 


402. 


263. 






401. 


- 356. 


P = '^-545 


Th 


387. 


- 134. 






377. 


- 354. 






327. 


50. 


P = '^-660 


Th 


360. 


-497. 


P = '^-640 


Th 


326. 


-339. 






293. 


129. 


P = '*-567 


Th 


253. 


596. 


P = 'l-541: 


vA 


250. 


480. 






249. 


- 61. 






217. 


259. 


P = '^-593 


Th 


198. 


377. 






216. 


66. 






236. 


- 337. 


P = ^-542 


Th 


185. 


398. 






193. 


239. 






166. 


450. 


P = ^-482 


vA 


145. 


655. 






155. 


368. 


P = '^-506 


J, Sh 


164. 


- 190. 






139. 


53. 


P-;|-663 


Th 


136. 


46. 


P = '^-519 


Th 


144. 


- 31. 


P = '^-548 


Sh, W 


112. 


565. 






101. 


159. 


P = '^-488 


vA 


64. 


46. 


P = ^-504: 


Sh,vA 


56. 


12. 


P='|-500 


Th 


12. 


438. 


P = '*-533 


J 


33. 


- 27. 


P = ^-587 


Th, Sh, W 


42. 


- 157. 






73. 


-441. 






23. 


693. 


P = S60 


Sh, vA 


20. 


- 158. 


P = '^-570 


Sh 


18. 


41. 


P = '^-531 


Sh 


6. 


-239. 






22. 


- 128. 






25. 


-247. 






42. 


33. 






71. 


237. 


P = ^-836 


vA 


50. 


- 231. 






23. 


- 372. 






75. 


92. 


P='^-618 


Th, vA 



218 



Publications of the David Dunlap Observatory 



TABLE V (continued) 



NR 



Period 



Remarks 



92 
93 
94 
95 
96 
97 
98 
99 
100 
101 
102 
103 
104 
105 
106 
107 
108 
109 
110 
111 
112 
113 
114 
115 
116 
117 
118 
119 
120 
121 
122 
123 
124 
125 
126 
127 
128 
129 
130 
131 
132 
133 
134 
135 
136 
137 



89. 


138. 


P = "-503 


vA 


97. 


381. 






80. 


- 186. 






84. 


5. 






99. 


7. 






102. 


- 41. 




red irr. 


96. 


- 232. 






112. 


- 165. 






141. 


105. 






152. 


162. 


P = '^-487 


vA 


172. 


321. 






169. 


292. 






214. 


- 98. 






228. 


39. 






410. 


306. 






195. 


183. 


P = ^-307 


Th 


86. 


- 108. 






137. 


176. 






206. 


- 397. 






248. 


- 80. 






232. 


-425. 






268. 


- 69. 






333. 


576. 






311. 


- 7. 






315. 


- 27. 






323. 


-302. 






371. 


406. 


P = l'^-15 




376. 


191. 


bright, Th, vA 


358. 


- 246. 






408. 


301. 






411. 


30. 






402. 


- 170. 


P = S66 


vA 


385. 


-469. 






460. 


- 249. 


P = '^-495 


vA 


538. 


343. 






508. 


-598. 






580. 


-345. 






614. 


171. 






690. 


413. 






687. 


-532. 






745. 


118. 






761. 


239. 






805. 


-466. 






895. 


- 316. 






819. 


354. 






749. 


629. 







The Sculptor Dwarf Spheroidal Galaxy 



219 



TABLE V (continued) 



NR 



X" 



Y" 



Period 



Remarks 



138 

139 

140 

141 

142 

143 

144 

145 

146 

147 

148 

149 

150 

151 

152- 

153 

154 

155 

156 

157 

158 

159 

160 

161 

162 

163 

164 

165 

166 

167 

168 

169 

170 

171 

172 

173 

174 

175 

176 

177 

178 

179 

180 

181 

182 



764. 


48. 


P = '^-619 


vA 


726. 


- 17. 






722. 


-207. 






700. 


31. 






585. 


716. 






514. 


462. 






535. 


- 93. 


P = ^-350 


vA 


558. 


- 61. 


P = ^-523 


Sh,W 


479. 


- 157. 






452. 


83. 






466. 


-262. 






487. 


-522. 






434. 


- 239. 






421. 


- 80. 






425. 


- 123. 






411. 


- 136. 






402. 


- 83. 






376. 


112. 


P = ^-550: 


Th 


355. 


97. 


P = ^-509 


Th 


344. 


133. 


P = ^-293 


Th 


378. 


-588. 






320. 


- 32. 


P = ^-672 


Th 


319. 


158. 


P = ^-5I5 


Th 


343. 


- 193. 






274. 


394. 






240. 


- 18. 






273. 


-283. 






166. 


731. 






213. 


- 14. 






212. 


-391. 






179. 


- 54. 






151. 


199, 






133. 


162. 






136. 


- 7. 






94. 


521. 






232. 


-765. 






75. 


445. 






115. 


-235. 






113. 


-315. 






70. 


- 140. 






52. 


- 32. 






45. 


- 20. 


P = '^-715 


vA 


10. 


437. 






43. 


- 121. 






66. 


375. 


P = '^-360 


Th 



220 



Publications of the David Dunlap Observatory 



TABLE V (continued) 



NR 



X" 



Y" 



Period 



Remarks 



183 
184 
185 
186 
187 
188 
189 
190 
191 
192 
193 
194 
195 
196 
197 
198 
199 
200 
201 
202 
203 
204 
205 
206 
207 
208 
209 
210 
211 
212 
213 
214 
215 
216 
217 
218 
219 
220 
221 
222 
223 
224 
225 
226 
227 
228 



25. 


- 36. 




5. 


-700. 




48. 


-571. 




102. 


239. 




126. 


668. 




113. 


282. 




110. 


36. 




124. 


47. 




139. 


- 16. 




93. 


-676. 




167. 


154. 




185. 


415. 




179. 


294. 




199. 


533. 




192. 


190. 




150. 


-492. 


P = ''-573 


220. 


165. 


236. 


556. 




159. 


-645. 




224. 


- 301. 




242. 


- 176. 




228. 


-526. 




357. 


494. 




337. 


38. 




386. 


- 15. 




371. 


-579. 




423. 


16. 




390. 


-536. 




459. 


72. 




489. 


- 105. 




481. 


-762. 




569. 


349. 




633. 


369. 




669. 


145. 




665. 


- 24. 




731. 


- 26. 




111. 


- 284. 




766. 


-612. 




822. 


-426. 




312. 


- 109. 




253. 


-327. 




287. 


225. 




469. 


- 151. 




132. 


174. 




689. 


89. 




535. 


- 240. 





vA 



The Sculp tor Dwarf Spheroidal Galaxy 22 1 

TABLE V (continued) 

NR X" Y" Period Remarks 



229 


- 77. 


- 135. 


230 


- 568. 


- 45. 


231 


- 79. 


66. 


232 


- 549. 


21. 


233 


- 23. 


345. 


234 


- 223. 


- 173. 


235 


524. 


- 47. 


236 


- 50. 


132. 


237 


- 69. 


257. 


238 


- 583. 


187. 


239 


176. 


448. 


240 


- 759. 


229. 


241 


- 32. 


241. 


242 


- 321. 


1224. 


243 


212. 


372. 


244 


134. 


1036. 


245 


193. 


1096. 


246 


- 909. 


- 945. 


247 


- 909. 


- 525. 


248 


- 779. 


- 448. 


249 


916. 


- 517. 


250 


- 990. 


- 10. 


251 


- 799. 


201. 


252 


- 1010. 


583. 


253 


- 876. 


766. 


254 


- 865. 


803. 


255 


- 1015. 


810. 


256 


- 702. 


1190. 


257 


- 515. 


- 256. 


258 


- 644. 


- 289. 


259 


- 484. 


472. 


260 


- 715. 


- 197. 


261 


- 59. 


- 1228. 


262 


- 464. 


444. 


263 


- 78. 


529. 


264 


- 128. 


4. 


265 


29. 


- 706. 


266 


36. 


- 691. 


267 


288. 


- 724. 


268 


106. 


- 206. 


269 


11. 


315. 


270 


843. 


- 561. 


271 


654. 


- 480. 


272 


392. 


757. 


273 


510. 


785. 


274 


715. 


570. 



P = d-642 vA 

P = ^-379: vA 



222 Publications of the David Dwilap Observatory 

TABLE V (continued) 

NR X" Y" Period Remarks 



275 

276 

277 

278 

279 

280 

281 

282 

283 

284 

285 

286 

287 

288 

289 

290 

291 

292 

293 

294 

295 

296 

297 

298 

299 

300 

301 

302 

303 

304 

305 1851. - 16. uncertain var. 

306 

307 

308 

309 

310 

311 

312 

313 

314 

315 

316 

317 

318 

319 

320 



1011. 


408. 


948. 


- 169. 


813. 


- 543. 


1038. 


- 827. 


959. 


6. 


747. 


337. 


883. 


404. 


997. 


521. 


720. 


648. 


934. 


676. 


772. 


nil. 


928. 


988. 


781. 


410. 


1130. 


- 474. 


1308. 


- 961. 


385. 


1039. 


204. 


- 389. 


45. 


130. 


106. 


- 78. 


755. 


- 20. 


494. 


- 250. 


569. 


180. 


847. 


188. 


889. 


75. 


290. 


225. 


764. 


589. 


1570. 


- 356. 


1556. 


84. 


1085. 


13. 


2881. 


277. 


1851. 


- 16. 


1700. 


23. 


2504. 


98. 


3173. 


1093. 


53. 


- 408. 


2. 


- 485. 


489. 


- 375. 


355. 


12. 


225. 


148. 


832. 


192. 


944. 


29. 


446. 


261. 


374. 


838. 


292. 


578. 


575. 


578. 


204. 


962. 



The Sculp tor Dwarf Spheroidal Galaxy 223 

TABLE V (continued) 

NR X" Y" Period Remarks 



321 


439. 


1158. 


322 


1463. 


875. 


323 


1769. 


1117. 


324 


3063. 


921. 


325 


564. 


- 942. 


326 


- 1297. 


- 1052. 


327 


- 2089. 


- 2059. 


328 


1690. 


- 543. 


329 


155. 


- 789. 


330 


- 250. 


- 529. 


331 


- 291. 


- 526. 


332 


- 312. 


- 899. 


333 


- 683. 


- 790. 


334 


- 1267. 


- 457. 


335 


- 1893. 


- 209. 


336 


- 1067. 


- 576. 


337 


237. 


- 1206. 


338 


- 3217. 


-2130. 


339 


- 581. 


- 2871. 


340 


982. 


115. 


341 


1283. 


275. 


342 


408. 


- 206. 


343 


- 288. 


1295. 


344 


- 152. 


2070. 


345 


376. 


- 451. 


346 


79. 


30. 


347 


- 398. 


265. 


348 


-1627. 


205. 


349 


- 841. 


- 329. 


350 


- 828. 


- 155. 


351 


263. 


- 256. 


352 


1116. 


- 149. 


353 


907. 


- 1010. 


354 


798. 


918. 


355 


600. 


1320. 


356 


- 653. 


1660. 


357 


- 574. 


1554. 


358 


1657. 


1990. 


359 


482. 


1958. 


360 


- 957. 


1952. 


361 


- 1809. 


1286. 


362 


- 1789. 


1210. 


363 


- 1568. 


369. 


364 


386. 


- 59. 


365 


228. 


- 243. 


366 


79. 


- 255. 



uncertain vai. 



224 



Publications of the David Diinlap Observatory 



TABLE V (continued) 



NR 



Y" 



Period 



Remarks 



367 


- 62. 


- 378. 


368 


51. 


- 131. 


369 


- 362. 


- 432. 


370 


92. 


- 552. 


371 


- 507. 


- 434. 


372 


- 866. 


- 446. 


373 


- 1354. 


- 790. 


374 


- 1731. 


- 1078. 


375 


- 2537. 


- 2028. 


376 


- 15. 


- 1109. 


377 


1905. 


- 1378. 


378 


- 638. 


- 2047. 


379 


- 2102. 


- 3723. 


380 


421. 


476. 


381 


97. 


1. 


382 


- 50. 


- 233. 


383 


- 13. 


118. 


584 


6. 


- 164. 


385 


134. 


- 229. 


386 


6. 


- 299. 


387 


- 299. 


- 70. 


388 


- 318. 


60. 


389 


- 578. 


39. 


390 


- 423. 


- 265. 


391 


- 208. 


1228. 


392 


- 288. 


653. 


393 


- 847. 


919. 


394 


352. 


679. 


395 


618. 


598. 


396 


357. 


372. 


397 


- 1998. 


159. 


398 


- 1659. 


6. 


399 


- 1139. 


262. 


400 


- 829. 


- 478. 


401 


- 717. 


494. 


402 


- 567. 


559. 


403 


- 484. 


195. 


404 


- 647. 


- 142. 


405 


- 593. 


- 104. 


406 


70. 


75. 


407 


34. 


3. 


408 


319. 


69. 


409 


377. 


142. 


410 


629. 


- 242. 


411 


734. 


32. 


412 


1859. 


23. 



uncertain var. 
uncertain var. 



uncertain var. 
uncertain var. 



The Sculptor Dwarf Spheroidal Galaxy 225 

TABLE V (continued) 

NR X" Y" Period Remarks 

413 
414 
415 
416 
417 
418 
419 
420 
421 
422 
423 
424 
425 
426 
427 
428 
429 
430 
431 
432 
433 
434 
435 
436 
437 
438 
439 
440 
441 
442 
443 
444 
445 
446 
447 
448 
449 
450 
451 
452 
453 
454 
455 
456 
457 
458 



3006. 


192. 


1008. 


- 227. 


837. 


43. 


177. 


- 744. 


430. 


- 618. 


509. 


- 828. 


55. 


- 606. 


761. 


- 622. 


942. 


- 994. 


470. 


- 952. 


634. 


- 882. 


623. 


- 901. 


778. 


- 150. 


88. 


- 442. 


10. 


27. 


153. 


- 1111. 


165. 


- 949. 


888. 


- 437. 


1078. 


- 264. 


825. 


- 1093. 


2033. 


244. 


107. 


- 440. 


543. 


381. 


173. 


- 380. 


1090. 


- 157. 


1151. 


- 164. 


166. 


- 682. 


43. 


- 616. 


235. 


- 613. 


1020. 


- 1067. 


2229. 


- 1141. 


3272. 


- 1258. 


2184. 


- 1913. 


7. 


208. 


65. 


218. 


39. 


154. 


49. 


311. 


625. 


- 78. 


355. 


11. 


95. 


- 114. 


69. 


54. 


58. 


11. 


982. 


- 27. 


1322. 


305. 


1047. 


615. 


418. 


517. 



226 



Publications of the David Dunlap Observatory 



TABLE V (continued) 



NR 



X" 



Period 



Remarks 



459 


- 591. 


126. 


460 


- 909. 


236. 


461 


- 3516. 


- 142. 


462 


- 13. 


478. 


463 


1056. 


487. 


464 


798. 


491. 


465 


164. 


859. 


466 


198. 


239. 


467 


366. 


39. 


468 


468. 


- 124. 


469 


274. 


- 77. 


470 


- 94. 


935. 


471 


- 91. 


1401. 


472 


- 69. 


1245. 


473 


- 555. 


1216. 


475 


- 308. 


123. 


476 


- 491. 


240. 


477 


- 366. 


- 304. 


478 


381. 


- 1042. 


479 


- 1838. 


-2335. 


480 


1479. 


- 1233. 


481 


- 784. 


- 20. 


482 


- 1519. 


576. 


483 


- 1823. 


634. 


484 


- 1459. 


- 828. 


485 


- 861. 


- 951. 


486 


1635. 


91. 


487 


1178. 


- 260. 


488 


1115. 


- 255. 


489 


978. 


303. 


490 


540. 


260. 


491 


486. 


215. 


492 


- 82. 


- 410. 


493 


205. 


- 413. 


494 


- 364. 


- 299. 


495 


- 674. 


- 539. 


496 


- 857. 


- 557. 


497 


- 307. 


1019. 


498 


- 102. 


31. 


499 


- 482. 


- 11. 


500 


- 410. 


434. 


501 


- 725. 


- 405. 


502 


- 780. 


- 358. 


503 


-2561. 


- 898. 


504 


- 480. 


562. 



The Sculptor Dwarf Spheroidal Galaxy 221 

TABLE V (continued) 

NR X" Y" Period Remarks 



505 


931. 


964. 


506 


775. 


719. 


507 


- 56. 


86. 


508 


- 246. 


- 56. 


509 


- 366. 


56. 


510 


- 602. 


- 198. 


511 


576. 


- 790. 


512 


733. 


- 243. 


513 


611. 


- 1911. 


514 


707. 


- 2389. 


515 


- 587. 


- 115. 


516 


- 659. 


- 364. 


517 


- 544. 


- 339. 


518 


- 220. 


- 50. 


519 


- 395. 


50. 


520 


- 1457. 


- 250. 


521 


- 1376. 


122. 


522 


- 355. 


- 424. 


523 


- 115. 


- 370. 


524 


103. 


- 395. 


525 


277. 


- 688. 


526 


165. 


- 429. 


527 


1033. 


457. 


528 


3627. 


1661. 


529 


1683. 


2025. 


530 


1941. 


1166. 


531 


1165. 


918. 


532 


449. 


873. 


533 


- 271. 


658. 


534 


- 958. 


689. 


535 


- 1585. 


818. 


536 


1441. 


- 249. 


537 


1637. 


- 129. 


538 


1313. 


32. 


539 


- 238. 


- 246. 


540 


603. 


- 318. 


541 


951. 


- 809. 


542 


924. 


316. 


543 


- 456. 


1068. 


544 


- 111. 


866. 


545 


280. 


435. 


546 


- 1472. 


- 879. 


547 


- 990. 


- 1218. 


548 


- 717. 


- 562. 


549 


- 311. 


- 75. 


550 


- 87. 


- 708. 



LP 



228 Publications of the David Dunlap Observatory 

TABLE V (continued) 

NR X" Y" Period Remarks 

551 
552 
553 
554 
555 
556 
557 
558 
559 

560 - 1788. 9110. f 

561 - 7014. 4894. f 

562 - 402. 4658. f 

563 - 1822. 4005. f 

564 1867. 4050. f 
565 
566 
567 
568 
569 
570 
571 
572 
573 
574 
575 
576 
577 
578 
579 
580 
581 
582 
583 
584 
585 
586 
587 
588 

589 - 866. -4293. f 

590 2839. - 3990. f 

591 4291. -5002. f 

592 -2817. -5650. f 

593 - 921. -6133. f 

594 7258. - 7025. f 
595 
596 



48. 


- 971. 


288. 


- 178. 


2638. 


- 202. 


407. 


816. 


1764. 


254. 


975. 


5. 


283. 


138. 


306. 


- 455. 


1401. 


215. 


1788. 


9110. 


7014. 


4894. 


402. 


4658. 


1822. 


4005. 


1867. 


4050. 


3900. 


2613. 


4722. 


2231. 


868. 


2039. 


637. 


760. 


3623. 


1934. 


531. 


740. 


1865. 


908. 


4150. 


1068. 


2626. 


873. 


434. 


25. 


352. 


302. 


24. 


372. 


2032. 


- 70. 


3547. 


241. 


2587. 


- 974. 


1820. 


- 668. 


1310. 


- 386. 


91. 


- 902. 


547. 


- 32. 


27 83. 


- 234. 


1155. 


- 570. 


3030. 


- 1954. 


2895. 


- 2235. 


544. 


- 3283. 


866. 


-4293. 


2839. 


- 3990. 


4291. 


- 5002. 


2817. 


- 5650. 


921. 


-6133. 


7258. 


- 7025. 


3721. 


- 6907. 


1708. 


521. 



The Sculptor Dwarf Spheroidal Galaxy 229 

TABLE V (continued) 

NR X" Y" Period Remarks 

597 
598 
599 
600 
601 
602 
603 



295. 


382. 


1486. 


- 809. 


1161. 


- 38. 


131. 


1030. 


4691. 


9683. 


274. 


113. 


2016. 


1127. 



230 Publications of the David Dunlap Observatory 






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PLATE I 

Identification of the variable stars in the central region of the sculptor dwarf spheroidal galaxy. 

The scale (60") is indicated in the upper right hand corner. 



The Sculptor Dwarf Spheroidal Galaxy 



231 









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PLATE II 
Identification of the variable stars in the NW quadrant. The scale (120") is indicated. 



232 



Publications of the David Dunlap Observatory 



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' • • ■ ■ '»' ,•. 



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PLATE III 

Identification of the variable stars in the NE quadrant. 



The Sculptor Dwarf Spheroidal Galaxy 233 






w. ^■;.^: 






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•♦ •• 



PLATE IV 
Identification of the variable stars in the SE quadrant. 



234 



Publications of the David Dunlap Observatory 



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PLATE V 

Identification of the variable stars in the SW quadrant. 



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The Sculptor Dwarf Spheroidal Galaxy 235 



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PLATE VI 

Identification of tiic majority of the variable stars in the outer regions of the Sculptor dwarf galaxy. 

The scale (10 arcmin) is indicated. 



90904^ 



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